Venus, with its thick and unique atmosphere, presents a prime location for observing meteors. Studies suggest that a Venus orbiter could significantly enhance our understanding of meteoroids and their properties, revealing insights about the composition and evolution of the solar system.
Summary
Observing meteors on Venus offers a new method to study meteoroids.
Venus’ thick atmosphere is ideal for detecting meteors.
Future Venus missions, like ESA’s EnVision, could include meteor observation tools.
Meteors on Venus could be brighter and more detectable than on Earth.
Meteor studies on Venus could provide critical data on the formation and composition of the solar system.
Introduction
Watching meteoroidsenter Earth’s atmosphere and create meteors is one of the most awe-inspiring spectacles on Earth. These fiery streaks often exhibit multiple colors, revealing their mineral compositions. But what if we could detect and observe meteors on other planets with atmospheres, like Venus? This concept, explored by a recent study, could help us better determine meteoroid compositions and sizes.
Motivation Behind the Study
The primary aim of the study discussed here is to measure the flux of solid particles in space. According to Dr. Apostolos Christou, an astronomer at the Armagh Observatory and Planetarium, “The smallest particles can be efficiently counted with small-area impact detectors mounted on spacecraft, while larger objects can be found with telescopes. However, anything between a couple of hundred microns and a meter falls into a gap.” The study aims to bridge this gap by observing meteors in the atmosphere of Venus, treating the planet as an area detector.
Study Methodology
Researchers used a survey simulation toolkit called SWARMS (Simulator for Wide Area Recording of Meteors from Space) to determine the feasibility of a camera onboard a future Venus orbiter observing meteors within Venus’ atmosphere. The simulation used meteoroid populations observed on Earth for Venus, along with atmospheric modeling and instrument types. They hypothesized a meteor camera onboard the upcoming European Space Agency’s EnVision orbiter.
Significant Findings
The study found that the number of meteors a Venus orbiter camera could observe in the Venusian atmosphere would be 1.5 to 2.5 times greater than on Earth. Dr. Christou notes, “Meteors at Venus occur well above the cloud layers and are consistently brighter than their Earth counterparts.” This suggests that any camera design that works in Earth orbit should perform as well, if not better, at Venus.
Follow-Up Studies and Future Plans
Future studies will explore various assumptions made in the initial study, such as the fixed altitude of the camera and the potential for observing meteors from an elliptical orbit. Dr. Christou also mentioned the possibility of detecting bright meteors (fireballs) from the ground with telescopes, similar to observations made on Jupiter.
Upcoming Missions
NASA’s VERITAS and ESA’s EnVision missions, planned for the next decade, aim to map Venus’ surface using advanced radar and spectroscopy tools. While these missions focus on surface mapping, there are no specific plans yet for a meteor observation camera. However, with international interest in Venus exploration, now is an ideal time to advocate for such an instrument.
Observing Meteors on Other Planets
While Venus was the focus of this study due to its thick atmosphere, the gas giants (Jupiter, Saturn, Uranus, and Neptune) also have thick atmospheres that could be used for meteor observation. Dr. Christou points out that in 1994, fragments of comet Shoemaker-Levy 9 were observed entering Jupiter’s atmosphere, demonstrating the feasibility of such observations.
The Scientific Value of Meteor Studies
Studying meteoroids and meteors helps scientists understand the composition and properties of planetary bodies, offering insights into the formation and evolution of the solar system. As Venus exploration expands, meteor studies could provide even more valuable data.
Dr. Christou concludes, “Meteors should be ubiquitous to planets and moons with appreciable atmospheres. For instance, one should expect to see meteors on Titan and even on Triton, Neptune’s largest moon.”
Conclusion
Observing meteors on Venus and other planets with thick atmospheres offers a unique opportunity to enhance our understanding of meteoroids and the broader solar system. Future missions could incorporate meteor observation tools, providing valuable scientific insights and helping to unravel the mysteries of our cosmic neighborhood.
Starlink, a satellite internet service by SpaceX, offers a viable alternative to traditional NBN in Australia, particularly in rural areas. This article explores its setup, performance, technical specifications, and overall value, with insights into its potential advantages and limitations.
Summary
Introduction: Overview of Starlink, its purpose, and the current state of internet in Australia.
Unboxing and Setup: Detailed description of what comes with the Starlink kit and step-by-step setup instructions.
Technical Specifications: Examination of the hardware and software features of Starlink.
Performance Testing: Real-world speed tests and performance analysis.
Comparison with NBN: Evaluation of how Starlink stacks up against the National Broadband Network.
Cost and Availability: Pricing details and availability in Australia.
Potential Use Cases: Best scenarios for using Starlink.
Conclusion: Final thoughts on the viability and future of Starlink in Australia.
Introduction
Starlink, developed by SpaceX, aims to provide high-speed internet access across the globe through a constellation of low Earth orbit (LEO) satellites. This service is particularly beneficial for remote and rural areas where traditional internet infrastructure is lacking or inefficient. In Australia, the National Broadband Network (NBN) has been the primary internet service provider, but it has faced criticism for its performance and coverage issues. Starlink offers a promising alternative, and this article delves into its setup, performance, and overall value.
Unboxing and Setup
What’s in the Box?
When you purchase a Starlink kit, you receive the following components:
Rectangular Dish: The primary receiver for satellite signals.
Router: Provides Wi-Fi connectivity.
Ethernet Cable: For direct connections.
Power Supply: To power the router and dish.
Mounting Base: For securing the dish in place.
Setting Up Starlink
Find an Optimal Location: Use the Starlink app to scan the sky and find a location with minimal obstructions.
Mount the Dish: Secure the dish on a high point, such as a roof or pole, to ensure a clear line of sight to the sky.
Connect the Components: Attach the dish to the router using the provided cable and power up the system.
Configure the App: Follow the app instructions to complete the setup and connect to the internet.
Technical Specifications
Hardware
Component
Specification
Dish
Rectangular, motorized, IP54 rated
Router
Wi-Fi capable, SpaceX logo
Cables
75 ft and 150 ft options
Power Supply
150 watts maximum
Software
Starlink App: Available on iOS and Android, helps with setup and monitoring.
Firmware Updates: Regular updates to improve performance and stability.
Performance Testing
Speed Tests
Real-world speed tests show varying results based on location and time of day. Here are some examples:
Starlink offers competitive speeds that can rival NBN, especially in rural areas where NBN’s infrastructure is lacking. The reliability of Starlink also tends to be higher due to its satellite-based nature, avoiding common issues with ground-based systems.
Cost Analysis
Service
Monthly Cost (AUD)
Setup Cost (AUD)
Data Cap
Starlink
$140
$450
1 TB priority
NBN
$100-$150
Varies
Unlimited
While Starlink’s upfront cost is higher, its month-to-month flexibility and lack of contracts make it an attractive option.
Cost and Availability
Pricing
Starlink is priced at $140 AUD per month with a hardware cost of $450 AUD. This includes up to 1 TB of priority data, after which speeds may be reduced.
Availability
Starlink is available across Australia, with particular emphasis on rural and underserved areas. The service can be ordered online through the Starlink website.
Potential Use Cases
Rural Areas
Starlink is ideal for rural areas where NBN coverage is sparse or non-existent. It provides a reliable and fast internet connection, essential for both personal and business use.
Emergency Situations
In cases of natural disasters or other emergencies where traditional internet services are disrupted, Starlink can provide a crucial communication lifeline.
Temporary Solutions
For new builds or temporary setups, Starlink offers a quick and efficient way to get online without the need for extensive infrastructure.
Conclusion
Starlink presents a compelling alternative to NBN in Australia, especially for those in rural or underserved areas. Its easy setup, competitive speeds, and month-to-month flexibility make it an attractive option. While it may not yet be the perfect solution for everyone, it offers a glimpse into the future of global internet connectivity.
Big Red Spot on Jupiter: A Historical Overview from the 1800s
Key Takeaways
Jupiter’s Great Red Spot (GRS) is a massive, long-lived storm larger than Earth. First observed in the 1600s, the GRS has a complex and debated history. The storm is an anti-cyclonic vortex with wind speeds exceeding 400 km/h. Historical records and modern simulations suggest the GRS we see today likely formed in the mid-1800s. New research combines historical data with computer simulations to explore the GRS’s formation mechanisms.
Summary
Jupiter’s GRS: A massive, iconic storm larger than Earth, observed since the 1600s.
First Observations: Early sightings by astronomers like Giovanni Cassini and others in the 1600s and 1700s.
Lost Track: The GRS wasn’t observed for 118 years until its reappearance in the mid-1800s.
Historical Records: Early drawings and observations provide valuable data on the GRS’s appearance and movement.
Modern Observations: Spacecraft like Voyager, Galileo, and Juno have provided detailed images and data.
Wind Shear: Jupiter’s atmosphere contains winds running in opposite directions, creating conditions for the GRS.
Simulations: Supercomputer simulations explore possible formation mechanisms of the GRS.
Conclusion: The GRS likely formed from a South Tropical Disturbance (STrD) around the mid-1800s, acquiring its current form over time.
The Great Red Spot on Jupiter: How It Probably Formed in the Early 1800s
Jupiter’s Great Red Spot (GRS) is one of the most fascinating and enduring features of our Solar System. This massive storm, larger than Earth, has been observed by astronomers for centuries, with its formation and longevity still a topic of debate. The GRS is an enormous anti-cyclonic storm, rotating counter-clockwise with wind speeds exceeding 400 km/h (250 mph). It’s a striking feature that has captivated humans since at least the 1800s, and possibly earlier. Understanding its history and formation requires a look at both historical observations and modern scientific research.
Early Observations of the Great Red Spot
The earliest observations of the GRS may date back to 1632 when a German Abbott used his telescope to observe Jupiter. Thirty-two years later, another astronomer reported seeing a large spot moving from east to west across the planet. By 1665, the renowned astronomer Giovanni Cassini examined Jupiter and noted the presence of a storm at the same latitude as the current GRS. Cassini and his contemporaries observed this storm continuously until 1713, referring to it as the Permanent Spot.
Despite these early records, the GRS disappeared from astronomical observations for 118 years, only to be rediscovered in 1831 by astronomer S. Schwabe. He observed a clear, oval structure at the same latitude, which many believe marks the first sighting of the current GRS. This gap in observations has led to questions about the continuity of the storm and its relation to the earlier Permanent Spot.
These images from the research show how the GRS formed. a is a drawing by T. E. R. Phillips in 1931–1932 of the STrD. The red arrows indicate the flow direction. The longitude scale is indicated. b and c are maps drawn from images taken by the New Horizons spacecraft. The yellow arrows mark position-velocity changes in the STrD. The STrD trapped winds. It created a long cell that generated the Great Red Spot. Image Credit: Sánchez-Lavega et al. 2024.
The Role of Historical Records
Historical records play a crucial role in understanding the GRS. Early drawings and descriptions by astronomers like Cassini provide valuable insights into the size, structure, and movement of the storm. However, interpreting these records is challenging due to the variable appearance of the GRS over time. Changes in size, albedo, and contrast with surrounding clouds have made it difficult to definitively link the Permanent Spot observed by Cassini with the current GRS.
A recent study in Geophysical Research Letters, led by Professor Agustín Sánchez-Lavega of the University of the Basque Country in Bilbao, Spain, attempts to bridge this gap. The research combines historical records with computer simulations to better understand the formation and evolution of the GRS.
Modern Observations and Technology
Modern technology has revolutionized our understanding of the GRS. Space telescopes and spacecraft have provided detailed images and data that were unimaginable in Cassini’s time. NASA’s Voyager 1 spacecraft captured the first detailed image of the GRS in 1979, revealing intricate wave patterns within the storm. Subsequent missions, including Galileo and Juno, have provided even more detailed observations.
Juno, in particular, has made significant contributions to our understanding of the GRS. Its close flybys of Jupiter have allowed scientists to capture high-resolution images and measure the depth of the storm. Juno’s instruments have shown that the GRS is relatively shallow, with a vertical extent of about 500 km, compared to its vast horizontal dimensions.
Jupiter’s atmosphere is characterized by powerful winds blowing in opposite directions at different latitudes. North of the GRS, winds blow westward at speeds of 180 km/h, while south of the storm, winds flow eastward at 150 km/h. This wind shear creates the conditions necessary for the formation and maintenance of the GRS.
Researchers have used supercomputer simulations to explore various mechanisms that could produce the GRS under these conditions. One hypothesis involves the eruption of a gigantic superstorm, similar to those observed on Saturn, while another suggests that smaller vortices created by wind shear merged to form the GRS. However, these simulations did not fully match the characteristics of the current GRS.
A New Hypothesis: The South Tropical Disturbance
A more promising explanation emerged from simulations involving the South Tropical Disturbance (STrD), an instability in Jupiter’s winds. The researchers found that the STrD could trap winds and create an elongated cell that eventually evolved into the GRS. This process likely began in the mid-1800s, when the GRS was much larger than it is today.
The simulations show that over time, the GRS would rotate more rapidly and become more compact as it shrank, eventually resembling the current storm. This hypothesis aligns with historical observations and modern data, suggesting that the GRS we see today is about 150 years old.
This research figure compares the Permanent Spot (PS) and today’s GRS. a, b, and c are Cassini’s drawings from 1677, 1690, and 1691. d is a 2023 GRS image. Image Credit: Sánchez-Lavega et al. 2024.
Detailed Analysis of Historical Observations
To support their hypothesis, the researchers analyzed historical records in detail. They compared drawings and descriptions of the Permanent Spot from the 1600s and 1700s with observations of the GRS from the 1800s onwards. They also examined photographs and telescopic images from the late 19th and early 20th centuries.
Table 1: Comparison of Historical Observations
Year
Observer
Description
Notes
1665
Giovanni Cassini
Large spot at GRS latitude
Named it the Permanent Spot
1831
S. Schwabe
Oval structure at GRS latitude
First modern observation of the GRS
1879
A. A. Common
Clear photograph of GRS
Confirms presence of a large storm
1890
Observatory Lick
Yellow filter photograph
Detailed image showing GRS structure
These historical records provide a timeline of the GRS’s appearance and changes over the centuries. By comparing these records with modern observations, researchers can better understand the storm’s evolution.
Modern Spacecraft Observations
Spacecraft missions have been instrumental in studying the GRS. NASA’s Voyager 1 provided the first detailed image in 1979, revealing the storm’s complex structure. The Galileo spacecraft, which orbited Jupiter from 1995 to 2003, captured additional images and data. More recently, the Juno spacecraft has provided the most detailed observations yet, including measurements of the storm’s depth and high-resolution images.
Table 2: Key Spacecraft Observations
Spacecraft
Year
Key Observations
Voyager 1
1979
First detailed image of GRS
Galileo
1995-2003
Extensive imaging and data collection
Juno
2016-Present
High-resolution images and depth measurements
These observations have provided critical data on the GRS’s structure, composition, and dynamics. They have also revealed changes in the storm over time, such as its shrinking size and increasing rotation speed.
The Future of GRS Research
As technology continues to advance, our understanding of the GRS will deepen. Future spacecraft missions and advanced telescopes will provide even more detailed observations, allowing scientists to study the storm in unprecedented detail. Additionally, improved computer simulations will help researchers test new hypotheses and refine existing models.
Conclusion
Jupiter’s Great Red Spot is a remarkable and enduring feature of our Solar System. Its formation and longevity have intrigued astronomers for centuries. By combining historical records with modern observations and simulations, researchers have developed a plausible explanation for the GRS’s formation in the mid-1800s. This iconic storm, with its swirling red clouds and powerful winds, continues to captivate scientists and the public alike.
NASA Delays Boeing’s Starliner Launch Landing to June 22
Key Takeaway:
Boeing’s Starliner spacecraft, carrying NASA astronauts Butch Wilmore and Suni Williams, will now return to Earth on June 22. The delay allows for additional testing and system checks on the International Space Station, providing critical data for future missions.
Summary:
Boeing’s Starliner launched on June 5 with astronauts Butch Wilmore and Suni Williams.
The spacecraft docked at the ISS on June 6.
The mission was originally planned for about a week but is now extended.
The new return date is set for June 22.
Additional tests and safety drills will be conducted.
Initial delay was due to ISS preparation for an EVA.
Further delay reasons will be discussed in a NASA briefing.
Key personnel: Steve Stich and Mark Nappi.
Detailed Article
On June 5, 2024, NASA astronauts Butch Wilmore and Suni Williams launched aboard Boeing’s Starliner spacecraft as part of the Crew Flight Test (CFT) mission. The mission, intended to validate the Spacecraft’s performance during a full on-orbit shakedown, saw the Starliner dock with the International Space Station (ISS) the following day. Originally set for a week-long duration, the mission will now extend until June 22, allowing for additional tests and data collection.
The Launch and Docking
The Crew Flight Test for Boeing’s Starliner spacecraft marks a significant milestone in NASA’s Commercial Crew Program. Launching on June 5 from Cape Canaveral, the spacecraft carried two seasoned NASA astronauts: Butch Wilmore and Suni Williams. The mission aimed to demonstrate Starliner’s capabilities and ensure its readiness for future long-term missions.
Upon docking with the ISS on June 6, the Starliner successfully integrated with the station, providing a robust platform for the astronauts to conduct tests and assessments. This docking not only validated the spacecraft’s automated rendezvous and docking systems but also set the stage for an extended stay and additional evaluations.
Delays and Their Implications
First Delay: Extravehicular Activity Preparation
Initially, the mission was scheduled to last about a week. However, on June 9, a delay was announced, pushing the return date to June 18. The primary reason for this delay was to allow ISS residents more time to prepare for an extravehicular activity (EVA) planned for June 13. Unfortunately, this EVA was canceled due to “spacesuit discomfort,” identified shortly before NASA astronauts Tracy Dyson and Matt Dominick were set to exit the station.
Second Delay: Extended Testing
The most recent delay, announced on June 17, extends the mission by an additional four days, moving the return date to June 22. While NASA did not immediately provide a direct reason for this delay, it is believed to offer a unique opportunity for additional testing and validation of Starliner’s systems.
Steve Stich, manager of NASA’s Commercial Crew Program, emphasized the importance of these extended tests:
With the extended stay, Wilmore and Williams will conduct several critical tests and drills. These include a “hot-fire” test of seven of the spacecraft’s eight aft thrusters and a review of hatch operations. Furthermore, they will perform “safe haven” drills to prepare the capsule for potential emergencies, enhancing their readiness for unforeseen situations.
Mark Nappi, vice president and program manager for Boeing’s Commercial Crew Program, expressed optimism about the extended mission:
“We have an incredible opportunity to spend more time at station and perform more tests which provides invaluable data unique to our position.”
Table 1: Key Events in the Starliner Mission
Date
Event
Details
June 5, 2024
Launch of Starliner
Launched with astronauts Butch Wilmore and Suni Williams
June 6, 2024
Docking with ISS
Successful docking with the ISS
June 9, 2024
First delay announced
Extended mission to June 18 due to EVA preparation
June 13, 2024
Planned EVA
EVA canceled due to spacesuit discomfort
June 17, 2024
Second delay announced
New return date set for June 22
Impact on Future Missions
Preparing for Long-Term Missions
The data gathered during this extended mission will be crucial for future operations. The tests and drills conducted will provide valuable insights into the Starliner’s performance in various scenarios, ensuring its readiness for longer, more complex missions.
Enhancing Safety Protocols
The “safe haven” drills and thruster tests are particularly significant as they enhance the safety protocols for future crews. These exercises help astronauts prepare for emergencies, ensuring they can respond effectively and safely.
Table 2: Starliner System Tests
Test
Purpose
Outcome Expected
Hot-fire test of thrusters
Validate thruster performance under load
Ensure reliable propulsion in critical maneuvers
Hatch operations review
Assess hatch functionality and ease of use
Confirm reliability for docking and undocking
Safe haven drills
Prepare for emergency scenarios
Enhance crew readiness for unforeseen situations
Future Prospects and Challenges
Collaboration with NASA and Boeing
The collaboration between NASA and Boeing is pivotal for the success of the Commercial Crew Program. Both organizations are committed to ensuring the Starliner meets all safety and performance standards. The additional time spent in orbit provides a valuable opportunity to refine the spacecraft’s systems and protocols.
Addressing Technical Issues
While the mission has faced delays, these are not uncommon in space exploration. Addressing technical issues and ensuring the safety of the crew are of paramount importance. The delays allow both NASA and Boeing to meticulously examine the spacecraft and make necessary adjustments.
Conclusion
The delay in Boeing’s Starliner mission to June 22 highlights the complexities and challenges of space exploration. While the delays may seem inconvenient, they provide essential opportunities to gather data, conduct tests, and enhance safety protocols. The collaboration between NASA and Boeing continues to push the boundaries of what is possible in human spaceflight, paving the way for future long-term missions to the International Space Station and beyond.
Mars Food Revolution: Aquatic Solutions Turning Regolith into Fertile Soil
Key Takeaway
The prospect of colonizing Mars is becoming increasingly realistic, and with it comes the challenge of sustainable food production. Recent research suggests that an aquaponic system, combining fish farming and hydroponics, could be the key to transforming Martian regolith into fertile soil, making self-sustaining agriculture on Mars a viable option.
Summary
Colonization Challenge: Sustaining a human colony on Mars requires local food production.
Aquaponic System: Combines fish farming with hydroponics to create a self-sustaining biosphere.
Nutrient-Rich Water: Water from fish tanks is rich in nutrients that can fertilize Martian regolith.
Research Findings: Studies show that vegetables can be grown in regolith fertilized by fish tank water.
Feasibility: Simulation of Martian environment shows promising results for aquaponic farming.
Fish and Plants: Tilapia fish and various vegetables were successfully grown in the study.
Sustainable Solution: Offers a practical alternative to expensive supply missions from Earth.
Astronaut on the alien planet. Stars above. The elements of this image furnished by NASA.
Introduction
In the next few decades, humanity may achieve one of its most ambitious goals: colonizing Mars. The red planet, 54.6 million kilometers away, presents numerous challenges, with one of the most pressing being sustainable food production. While supply missions from Earth could be an option, they are not cost-effective or sustainable in the long term. Thus, the key to a successful Martian colony lies in local food production, and recent research suggests that an aquaponic system could provide the solution.
Mars is an unforgiving environment. With an atmosphere composed of 95% carbon dioxide, harsh weather conditions, and soil that lacks organic material, growing food seems like an insurmountable task. In the movie “The Martian,” Matt Damon’s character, Dr. Mark Watney, grows potatoes in regolith fertilized with human waste. While this made for a compelling story, real-life solutions may need to be less risky and more practical.
Researchers have turned their attention to aquaponics, a system that combines aquaculture (raising fish) and hydroponics (growing plants without soil). This system can create a self-sustaining biosphere, where nutrient-rich water from fish tanks is used to fertilize plants. This method holds promise not only for Mars but also for arid and inhospitable regions on Earth.
Research and Findings
To explore the feasibility of this system on Mars, a team of researchers set up an aquaponic system in a controlled environment simulating Martian conditions. They used tilapia fish and a variety of vegetables, including potatoes, tomatoes, beans, and carrots.
The researchers constructed a tent that mimicked the Martian environment, providing the necessary light and environmental stimuli for the fish and plants. The nutrient-rich water from the fish tanks was used to irrigate the plants, and the results were promising.
Results
The study showed that the nutrient-rich water from the fish tanks significantly improved the quality of the Martian regolith, turning it into a medium capable of supporting plant life. Vegetables not only grew but thrived in this environment, demonstrating the potential of this method for future Mars colonies.
Practical Applications
The benefits of this research extend beyond Mars. The same aquaponic systems could be used in environmentally hostile regions on Earth, providing a sustainable solution for food production in arid and nutrient-poor areas.
Table 1: Comparison of Aquaponic Systems on Earth and Mars
Feature
Earth
Mars
Environment
Varied
Simulated Martian conditions
Water Source
Freshwater
Ice extraction or transported
Nutrient Source
Fish waste
Fish waste
Plant Growth
High yield
High yield
Soil Improvement
Fertile soil from regolith
Fertile soil from regolith
Light Source
Natural and artificial
Artificial (LEDs)
Temperature Control
Easier to maintain
Challenging but manageable
For Mars colonization, the scalability of this system is crucial. Aquaponics can be scaled up or down depending on the colony’s size and needs. Additionally, it offers a closed-loop system where waste from the fish provides nutrients for the plants, which in turn purify the water for the fish.
Table 2: Benefits of Aquaponics for Mars Colonization
Benefit
Description
Sustainability
Provides a continuous supply of fresh produce and fish
Resource Efficiency
Uses less water compared to traditional farming
Soil Fertility
Enhances the nutrient content of Martian regolith
Environmental Control
Can be optimized for the harsh Martian environment
Reduced Dependence on Earth
Less reliance on supply missions, lowering costs and increasing self-sufficiency
Versatility
Suitable for various plant and fish species
Challenges and Solutions
Water Management
One of the primary challenges of aquaponics on Mars is water management. While Mars has water ice, extracting and purifying it will require advanced technology. Once extracted, maintaining a closed-loop system will be essential to minimize water loss.
Light and Temperature Control
Mars receives less sunlight than Earth, and its temperatures are much colder. Therefore, artificial lighting (e.g., LEDs) and temperature control systems are necessary. These systems must be energy-efficient and capable of supporting plant and fish growth.
Regolith Improvement
While the study shows promising results, further research is needed to fully understand the long-term effects of using Martian regolith as a growing medium. Continuous improvement and monitoring of soil quality will be vital to ensure sustainable crop yields.
Future Prospects
Technological Advancements
Advances in biotechnology, water purification, and renewable energy will play a crucial role in the success of aquaponics on Mars. Innovations in these fields will improve the efficiency and sustainability of the system.
Integration with Other Systems
Aquaponics can be integrated with other life support systems, such as bioregenerative life support, which uses plants to recycle air and water. This integration will create a more robust and self-sufficient colony.
Education and Training
Future colonists will need extensive training in aquaponics and other sustainable farming techniques. Educational programs and simulations on Earth will prepare astronauts for the challenges of farming on Mars.
Conclusion
The dream of colonizing Mars is becoming closer to reality, but it comes with significant challenges. Sustainable food production is one of the most critical issues to address. The research into aquaponic systems offers a promising solution, demonstrating that it is possible to transform Martian regolith into fertile soil using nutrient-rich water from fish tanks. This system not only holds potential for Mars but also offers solutions for food production in hostile environments on Earth.
As we prepare for the next giant leap for mankind, innovative solutions like aquaponics will be at the forefront, ensuring that future Martian colonies are self-sustaining and capable of thriving in one of the most challenging environments imaginable.
The Future of Apple Development: Apple’s Message via Satellite Works Like iMessage and Free to Start With
Key Takeaways
Apple is expanding its satellite services with iOS 18 to include Message via satellite. Initially, Message via satellite will be free, but future costs are uncertain. The service will be available on iPhones with existing satellite connectivity. Message via satellite will support standard text messaging features like Tapback reactions and emojis. The service is intended for non-emergency use, allowing users to stay connected in remote areas.
Summary
Emergency SOS via Satellite: Successful feature since late 2022.
Expansion with iOS 18:Satellite text messaging services.
Messaging Features: Similar to iMessage, supports Tapback reactions and emojis.
Usage: Non-emergency, regular text messaging.
Initiating Conversations: Users must initiate satellite SMS conversations.
RCS Messaging: Not supported due to satellite transfer limits.
Introduction
Apple’s commitment to innovation continues with the expansion of its satellite services. Following the success of Emergency SOS via satellite, Apple is set to introduce Message via satellite with the release of iOS 18. This new feature will allow users to send text messages via satellite, ensuring connectivity in remote areas where traditional cellular networks are unavailable. Initially free, this service is designed to provide a seamless messaging experience similar to iMessage.
Emergency SOS via Satellite: A Game Changer
Since its launch in late 2022, Emergency SOS via satellite has proven to be a critical feature for iPhone users. It allows people in distress to contact emergency services even when they are out of cellular range. This service has already saved numerous lives, highlighting the importance of reliable communication in emergencies. Given its success, Apple decided to expand its satellite capabilities to include regular text messaging.
Expansion with iOS 18
With the upcoming iOS 18 update, Apple will introduce Message via satellite. This feature builds on the technology used for Emergency SOS but is designed for everyday use. Users will be able to send and receive text messages, ensuring they can stay in touch with friends and family even in the most remote locations.
Free Service: At Least for Now
One of the key benefits of Emergency SOS via satellite has been its cost—or rather, the lack thereof. Apple initially offered the service for free for a year, later extending this to two years. As for Message via satellite, Apple has confirmed that it will also be free “at least for now.” However, the company has not provided details on potential future costs. This mirrors the uncertainty surrounding the pricing of Emergency SOS via satellite, which remains free with no announced plans for future charges.
No Special Hardware Required
Another significant advantage of Message via satellite is that it does not require any special hardware. According to Apple, the feature will be available through a software update for phones that already have satellite connectivity. This includes the iPhone 14, iPhone 15, and presumably the upcoming iPhone 16. This approach ensures that a broad user base can access the service without needing to purchase new devices.
Supported Models
The following iPhone models will support Message via satellite:
iPhone 14
iPhone 15
iPhone 16 (expected)
These models are equipped with the necessary hardware to connect to satellites, making them capable of using this new feature.
Messaging Features: Familiar and Functional
Message via satellite aims to offer a messaging experience similar to iMessage. Users can expect familiar features such as Tapback reactions and emoji support. However, due to the nature of satellite communication, there will be some limitations. For instance, large files like videos and images will likely not be supported to prevent clogging up bandwidth.
Usage: Non-Emergency Communication
Unlike Emergency SOS via satellite, Message via satellite is intended for non-emergency use. This means users can text friends and family as they would with any other messaging service. This is particularly useful for staying connected in areas where traditional cellular service is unavailable.
Initiating Conversations
One important aspect of Message via satellite is that users must initiate conversations. While emergency contacts can message users freely via SMS, other contacts will not be able to do so unless the user initiates the conversation first. This ensures that satellite bandwidth is used efficiently and prevents unsolicited messages from clogging the system.
RCS Messaging: Not Supported
It is worth noting that RCS (Rich Communication Services) messaging will not be supported when iOS 18 launches. This is because RCS has not been optimized for the smaller transfer limits of satellite messaging. Apple may consider adding RCS support in the future if technological advancements allow.
Conclusion
Apple’s introduction of Message via satellite with iOS 18 marks a significant expansion of its satellite services. Building on the success of Emergency SOS via satellite, this new feature will allow users to stay connected in remote areas without cellular coverage. Initially free, Message via satellite offers a familiar messaging experience with features like Tapback reactions and emojis. While some limitations exist, such as the need to initiate conversations and the lack of RCS support, the service promises to be a valuable addition for iPhone users. As Apple continues to innovate, the future of satellite messaging looks bright.
Table 1: Comparison of Emergency SOS and Message via Satellite
Feature
Emergency SOS via Satellite
Message via Satellite
Initial Cost
Free
Free
Future Cost
Unknown
Unknown
Supported Devices
iPhone 14, 15, 16
iPhone 14, 15, 16
Use Case
Emergency
Non-emergency
Messaging Features
Limited
Tapback, Emojis
File Transfer
No
No
SMS Support
Yes
Yes
RCS Support
No
No
Table 2: Supported iPhone Models for Satellite Messaging
Galileo Second Generation Satellite Design Gets Green Light
Key Takeaways
Galileo Second Generation satellites have passed Critical Design Review boards. The new G2 fleet will bring enhanced navigation and timing capabilities. Two satellite families are being developed by Thales Alenia Space and Airbus Defence and Space. Production is accelerating with the aim to start launching before the end of the decade. Galileo currently serves over four billion smartphone users globally. The program is a flagship of the EU, managed and funded by the European Commission.
Summary
Galileo Second Generation (G2):
Two satellite designs passed Critical Design Review.
First board met on April 18 for Thales Alenia Space.
Second board met on May 16 for Airbus Defence and Space.
Boards included senior experts from ESA, EUSPA, and the European Commission.
Designs are robust and meet all mission and performance requirements.
Advanced Capabilities:
Fully digital navigation payloads.
Electric propulsion.
More powerful navigation antenna.
Inter-satellite link capacity.
Advanced atomic clock configuration.
High degree of flexibility.
Production and Testing:
Manufacturing of onboard equipment and satellite structures in progress.
Assembly and integration of components in proto-flight models to begin soon.
Second Generation launches to begin before the end of this decade.
Galileo’s Impact:
Most precise satellite navigation system globally.
Serves over four billion smartphone users.
Applications in rail, maritime, agriculture, financial timing services, and rescue operations.
Managed by the European Commission, developed by ESA, and services provided by EUSPA.
Detailed Article
The Galileo Second Generation (G2) satellite design has received approval from two independent Satellite Critical Design Review (CDR) boards, marking a significant milestone in the development of the next fleet of Galileo satellites. These new satellites promise to bring unprecedented advancements in positioning, navigation, and timing, supporting a wide array of user needs and services.
Critical Design Review Success
The two satellite families being developed by Thales Alenia Space and Airbus Defence and Space recently underwent thorough assessments by ESA-led CDR boards. These reviews, conducted on April 18 and May 16 respectively, verified the robustness and technical capabilities of the satellite designs.
Eric Villette and Alberto Bramante, who manage the G2 Space Segment contracts, elaborated on the CDR process. “It is structured around peer review panels led by independent technical experts from ESA specialized in satellite design,” said Villette. Bramante added, “The review is based on design descriptions, analyses, test plans, and test results provided by the industrial consortia.”
Advanced Capabilities of G2 Satellites
The Galileo Second Generation satellites will be groundbreaking in their design and functionality. They will feature:
Fully digital navigation payloads: Enhancing the accuracy and reliability of navigation services.
Electric propulsion: Offering more efficient and longer-lasting satellite operation.
Powerful navigation antenna: Providing stronger and more precise signals.
Inter-satellite link capacity: Allowing the satellites to communicate with each other, improving overall system performance.
Advanced atomic clock configuration: Ensuring highly accurate timing, crucial for navigation and synchronization services.
Flexible architecture: Adapting to various mission needs and evolving technological advancements.
Production and Testing Advancements
With the CDR approval, production of the Galileo Second Generation satellites is moving forward at full speed. Industry teams are currently busy manufacturing the onboard equipment and satellite structures. Soon, the components will be assembled and integrated into proto-flight models.
In the coming months, the first satellite compatibility test campaigns will be conducted. These tests are critical for validating the communication between the satellites and the ground segment, ensuring seamless operation once the satellites are in orbit.
Management and Coordination
Miguel Manteiga, Head of the Galileo Programme Office, expressed his gratitude to all the teams involved in the satellite CDR process. “It is remarkable to see how, when faced with the most exigent requirements for GNSS satellite systems in history, European industry can answer in time to deliver a state-of-the-art design,” he said. “We are really looking forward to ramping up manufacturing and to starting the System Compatibility Test campaigns with satellites, ground segment, and Galileo receivers.”
Current and Future Constellation
The current Galileo constellation comprises 30 First Generation satellites, with an additional eight ready for launch. The next two satellites are scheduled for launch in September this year, followed by six more starting in 2025. The launch of the Second Generation satellites is expected to begin before the end of this decade, paving the way for enhanced navigation services.
The Galileo System
Galileo is renowned for being the world’s most precise satellite navigation system. Since its Open Service launch in 2017, it has been serving over four billion smartphone users globally. The system has made significant impacts in various fields including rail, maritime, agriculture, financial timing services, and rescue operations.
Program Management and Funding
As a flagship program of the European Union, Galileo is managed and funded by the European Commission. The European Space Agency (ESA) is responsible for the design, development, and qualification of the space and ground systems, as well as procuring launches. ESA is also entrusted with research and development activities for the future of Galileo within the EU’s Horizon Europe program. The EU Agency for the Space Programme (EUSPA) acts as the service provider, overseeing market and application needs and closing the loop with users.
Impact and Applications
Galileo’s precise navigation capabilities have revolutionized various sectors:
Rail and Maritime: Enhancing safety and efficiency in transportation.
Agriculture: Supporting precision farming techniques, leading to higher yields and sustainable practices.
Financial Timing Services: Providing accurate timing for financial transactions and operations.
Rescue Operations: Facilitating faster and more accurate location of distressed individuals.
Conclusion
The approval of the Galileo Second Generation satellite designs marks a significant step forward in the evolution of the Galileo navigation system. With advanced capabilities and robust design, the new satellites promise to enhance navigation services and support a wide range of applications. As production ramps up and testing begins, the anticipation for the launch of the Second Generation satellites grows, heralding a new era in satellite navigation.
Tables
Table 1: Key Milestones of Galileo Second Generation
The Science Behind Liquid Water on Mars: Missions to Mars.
Key Takeaway
Understanding the presence and accessibility of liquid water on Mars is crucial for the success of future crewed missions. Despite some recent findings, the existence of liquid water on Mars remains a subject of debate.
Summary
NASA and China are planning crewed missions to Mars in the coming decades.
In-situ resource utilization (ISRU) is essential for sustaining astronauts on Mars.
Historical missions have revealed surface features suggesting past water flow on Mars.
ESA’s Mars Express detected bright radar reflections beneath the southern polar ice cap.
The MARSIS instrument found bright patches that could indicate liquid water.
Recent research suggests these reflections might be due to ice composition and layer thickness.
Liquid water on Mars would need to be very briny or heated by magma.
Future missions might need to rely on ice deposits or chemical reactions for water.
Findings about Mars’s geological activity suggest it may still be geologically active.
The possibility of microbial life existing on Mars remains a tantalizing prospect.
The Science Behind Liquid Water on Mars: Missions to Mars
In the coming decades, NASA and China intend to send the first crewed missions to Mars. Given the distance involved and the time it takes to make a single transit (six to nine months), opportunities for resupply missions will be few and far between. As a result, astronauts and taikonauts will be forced to rely on local resources to meet their basic needs – a process known as in-situ resource utilization (ISRU). For this reason, NASA and other space agencies have spent decades scouting for accessible sources of liquid water.
Finding this water is essential for future missions and scientific efforts to learn more about Mars’s past, when the planet was covered by oceans, rivers, and lakes that may have supported life. In 2018, using ground-penetrating radar, the ESA’s Mars Express orbiter detected bright radar reflections beneath the southern polar ice cap that were interpreted as a lake. However, a team of Cornell researchers recently conducted a series of simulations that suggest there may be another reason for these bright patches that do not include the presence of water.
Historical Evidence of Water on Mars
When the first robotic probes began making flybys of Mars in the 1960s, the images they acquired revealed surface features common on Earth. These included flow channels, river valleys, lakebeds, and sedimentary rock, all of which form in the presence of flowing water. For decades, orbiters, landers, and rovers have explored Mars’ surface, atmosphere, and climate to learn more about how and when much of this surface water was lost. In recent years, this has led to compelling evidence that what remains could be found beneath the polar ice caps today.
The most compelling evidence was obtained by the Mars Advanced Radar for Subsurface and Ionosphere Sounding (MARSIS) instrument aboard the Mars Express orbiter. This instrument was designed by NASA and the Italian Space Agency (ASI) to search for water on the Martian surface and down to depths of about 5 km (3 mi). The radar returns indicated that the bright patches could be caused by layered deposits composed of water, dry ice, and dust. These South Polar Layered Deposits (SPLD) are thought to have formed over millions of years as Mars’ axial tilt changed.
Subsequent research by scientists at NASA’s Jet Propulsion Laboratory (JPL) revealed dozens of other highly reflective sites beneath the surface. The implications of these findings were tremendous, not just for crewed missions but also for astrobiology efforts. In addition to being a potential source of water for future missions, it was also theorized that microbial life that once existed on the surface might be found there today. However, the findings were subject to debate as other viable explanations were offered.
The Debate on Liquid Water
While the same bright radar reflections have detected subglacial lakes on Earth (such as Lake Vostok under the East Antarctic Ice Sheet), Mars’s temperature and pressure conditions are very different. To remain in a liquid state, the water would need to be very briny, loaded with exotic minerals, or above an active magma chamber – none of which have been detected. As Lalich said in a recent interview with the Cornell Chronicle:
Research and Simulations
In a previous study, Lalich and his colleagues used simpler models to demonstrate that these bright radar signals could result from tiny variations in the thickness of the layers. These variations would be indiscernible to ground-penetrating radar and could lead to constructive interference between radar waves, producing reflections that vary in intensity and variability – like those observed across the SPLD. For their latest study, the team simulated 10,000 layering scenarios with 1,000 variations in the ice thickness and dust content of the layered deposits.
Their simulations also excluded any of the unusual conditions or exotic materials that would be necessary for liquid water. These simulations produced bright subsurface signals consistent with observations made by the MARSIS instrument. According to Lalich, these findings strongly suggest that he and his colleagues were correct in suspecting radar interference. In essence, radar waves bouncing off of layers too close together for the instrument to resolve may have combined, amplifying their peaks and troughs and appearing much brighter.
Implications for Future Missions
The team is not prepared to rule out the possibility that future missions with more sophisticated instruments could find definitive evidence of water. However, Lalich suspects that the case for liquid water (and potential life) on Mars may have ended decades ago.
If so, future missions may be forced to melt polar ice deposits and permafrost to get drinking water or possibly chemical reactions involving hydrazine (a la Mark Watney). In addition, astrobiology efforts may once again be placed on the back burner as they were when the Viking Landers failed to find conclusive evidence of biosignatures in 1976. But as we’ve learned, Mars is full of surprises. While the results of the Viking biological experiments were disappointing, these same missions provided some of the most compelling evidence that water once flowed on Mars’ surface.
Mars’ Geological Activity
Moreover, scientists once suspected that the Red Planet was geologically dead, but data obtained by NASA’s InSight Lander showed that it is actually “slightly alive.” This included evidence that hot magma still flows deep in the planet’s interior and that a massive magma plume still exists beneath the Elysium Planitia region, which may have caused a small eruption just 53,000 years ago (the most recent in Martian history). Perhaps the same will hold true for briny patches of liquid water around the poles and the equatorial region.
Potential for Microbial Life
With any luck, some of these patches may even house countless microorganisms that could be related to life on Earth. The possibility of finding life on Mars, even if it is microbial, would have profound implications for our understanding of biology and the potential for life elsewhere in the universe. How cool would that be?
The quest to find liquid water on Mars is ongoing and fraught with challenges. While recent findings cast doubt on the presence of liquid water, the pursuit has led to a deeper understanding of the planet’s geology and climate. Future missions will continue to explore this enigmatic planet, with the hope of uncovering the secrets that lie beneath its surface. Whether or not we find liquid water, the journey itself will expand our knowledge and pave the way for human exploration.
Warp Drive ERP: How Warp Drives Could Generate Gravitational Waves
Key Takeaways
Warp drives have a theoretical basis in general relativity. Miguel Alcubierre proposed the concept of warp drives in 1994. Warp drives could theoretically enable faster-than-light (FTL) travel by warping spacetime. Warp drives face significant scientific barriers, including energy requirements and stability issues. The collapse of a warp drive could potentially emit gravitational waves. Current gravitational wave detectors may not be sensitive enough to detect these signals. Future advancements in gravitational wave detection could potentially identify warp drive signals.
Summary
Warp drives, theoretically described by Alcubierre, offer a method of faster-than-light travel by warping spacetime.
The concept faces practical barriers, including the Null Energy Condition and stability issues.
Warp drives, a concept popularized by science fiction, have a theoretical foundation in general relativity. Proposed by Mexican physicist Miguel Alcubierre in 1994, warp drives could theoretically enable faster-than-light travel by warping spacetime.
Theoretical Basis of Warp Drives
The Alcubierre Drive proposes a method for faster-than-light travel by contracting spacetime in front of a spacecraft and expanding it behind. This would create a “warp bubble” that allows the spacecraft to travel faster than light without violating the principles of relativity.
Null Energy Condition
One major obstacle to creating a warp drive is the Null Energy Condition (NEC), which states that a region of space cannot have a negative energy density. While theoretical workarounds exist, none are currently practical.
Stability Issues
Another significant challenge is maintaining the stability of the warp bubble. While the Einstein Equation can initiate a warp bubble, no known equation can sustain it. The warp bubble tends to disperse or collapse into a central point.
Detecting Warp Drive Collapses
Gravitational Waves
Gravitational waves are ripples in spacetime caused by massive objects accelerating. The collapse of a warp drive could theoretically generate gravitational waves, similar to those produced by black hole mergers or neutron star collisions.
Simulation Results
Researchers simulated the collapse of a warp bubble and found that it generates a gravitational wave signal distinct from typical binary mergers. The signal comes as a burst, followed by an oscillatory period with a characteristic frequency.
Current and Future Detection
Current gravitational wave detectors, like LIGOand Virgo, may not be sensitive enough to detect the gravitational waves from a warp drive collapse. These detectors are designed to pick up signals within a specific frequency range, and warp drive signals may fall outside this range.
Future Advancements
Proposals for higher frequency gravitational wave detectors have been made, which could potentially detect warp drive signals in the future. These advancements would allow scientists to put bounds on the existence of such signals and explore the feasibility of warp drives further.
Multimessenger Signals
In addition to gravitational waves, the collapse of a warp drive could send multimessenger signals. However, it’s difficult to predict how the matter from a warp drive would interact with regular matter.
Theoretical Implications
The research into warp drives and their potential gravitational wave signals is still in its early stages. The current models have several theoretical problems that need to be addressed. Future research will focus on understanding the signatures of warp drive signals and characterizing their detectability.
Conclusion
Warp drives remain a fascinating theoretical concept with the potential to revolutionize space travel. While significant scientific barriers exist, ongoing research continues to explore their feasibility and implications. The detection of gravitational waves from warp drive collapses could provide valuable insights into the nature of spacetime and the possibilities of faster-than-light travel.
Tables
Table 1: Key Scientific Barriers to Warp Drives
Barrier
Description
Null Energy Condition (NEC)
States that a region of space cannot have a negative energy density
Stability Issues
Maintaining a stable warp bubble over time is currently not feasible
Energy Requirements
Theoretical models require enormous amounts of energy to create a warp bubble
NASA’s Edward C. Stone, Voyager Visionary, Dies at 88
Key Takeaways
Edward C. Stone, a luminary in space exploration and former director of NASA’s Jet Propulsion Laboratory, passed away on June 9, 2024, at age 88. Known for his leadership of the Voyager mission, Stone enhanced our understanding of the solar system and interstellar space. He also held a significant academic role at Caltech and received numerous accolades, including the National Medal of Science.
Stone served as the director of NASA’s Jet Propulsion Laboratory (JPL) from 1991 to 2001. He contributed to nine NASA missions as principal investigator or science instrument lead. Stone’s work on Voyager helped reveal significant discoveries about Jupiter, Saturn, Uranus, and Neptune. Under his leadership, Voyager 1 and Voyager 2 became the first human-made objects to enter interstellar space.He w as instrumental in engaging the public with scientific discoveries. Stone received numerous awards, including the National Medal of Science and the Shaw Prize in Astronomy.
Summary
Edward C. Stone, a prominent space scientist, died on June 9, 2024, at age 88.
He led the Voyager mission, NASA’s longest-running mission, which launched in 1977.
He was the director of NASA’s Jet Propulsion Laboratory from 1991 to 2001.
Stone was involved in multiple NASA missions, including the Parker Solar Probe and Cassini.
He was a professor at Caltech and served as vice provost for special projects.
Stone received numerous accolades, including the National Medal of Science and the Shaw Prize in Astronomy.
He is survived by his two daughters, Susan and Janet, and two grandsons.
Stone was known for his ability to engage the public with scientific discoveries.
Remembering Edward C. Stone
Edward C. Stone, former director of NASA’s Jet Propulsion Laboratory (JPL) and longtime project scientist of the agency’s Voyager mission, died on June 9, 2024, at the age of 88. He was preceded in death by his wife, Alice Stone, whom he met at the University of Chicago. They are survived by their two daughters, Susan and Janet Stone, and two grandsons.
Early Life and Education
Edward Carroll Stone Jr. was born on January 23, 1936, in Knoxville, Iowa. The eldest of two sons of Edward Carroll Stone Sr. and Ferne Elizabeth Stone, he grew up in the nearby commercial center of Burlington. His father was a construction superintendent who delighted in showing his son how to take things apart and put them back together again. This early exposure to mechanics fostered Stone’s curiosity and passion for understanding the world around him.
After high school, Stone enrolled in Burlington Junior College to study physics and went on to the University of Chicago for graduate school. Shortly after he was accepted, the Soviet Union launched Sputnik, marking the beginning of the Space Age. Stone joined a team at the university that was building science instruments to launch into space.
During their journeys, the spacecraft revealed significant discoveries, such as the first active volcanoes beyond Earth on Jupiter’s moon Io and an atmosphere rich with organic molecules on Saturn’s moon Titan. Voyager 2 remains the only spacecraft to fly by Uranus and Neptune, revealing Uranus’ unusual tipped magnetic poles and the icy geysers erupting from Neptune’s moon Triton.
Now more than 15 billion miles (24 million kilometers) from Earth, Voyager 1 is the most distant human-made object. Voyager 2, traveling slightly slower and in a different direction, is more than 12 billion miles (20 billion kilometers) from Earth. Both probes are exploring interstellar space, the region outside the heliosphere, which is a protective bubble created by the Sun’s magnetic field and the outward flow of charged particles.
“Becoming Voyager project scientist was the best decision I made in my life,” Stone said in 2018. “It opened a wonderful door of exploration.”
Ed Stone became project scientist for the Voyager mission in 1972. This was five years before launch. He served in the role for a total of 50 years. During that time, he also served as director of NASA’s Jet Propulsion Laboratory. This laboratory manages the Voyager mission for the agency. Credit: NASA/JPL-Caltech
Stone was particularly proud of the way Voyager quickened the pace of scientific analysis and took advantage of opportunities to engage the public. When Voyager 1 and 2 made their close flybys of the giant planets between 1979 and 1989, Stone was overseeing 11 teams of scientists, all accustomed to releasing their results at a slower pace through peer-reviewed journals.
Stone took the lead in tailoring the peer-review process to the faster pace of the mission’s planetary encounters. In the early afternoon, after data had come down, teams of scientists would decide what they thought their best results were for the day and hold up their conclusions for feedback in front of the whole science steering group. Based on that discussion, Stone would choose the most interesting results to present to the media and the public the next morning.
“It was a very exciting time, and everyone was making discoveries,” said Stamatios “Tom” Krimigis of the Johns Hopkins Applied Physics Laboratory. “Ed’s approach showed us how much public interest there really was in what Voyager was doing, but it also resulted in better science.”
Voyager’s high profile lifted Stone’s profile as well. In 1991, roughly two years after the mission completed its planetary flybys, Stone became director of JPL, serving until 2001. Under his leadership, JPL was responsible for more than two dozen missions and instruments. Highlights of Stone’s tenure included landing NASA’s Pathfinder mission with the first Mars rover, Sojourner, in 1996 and launching the NASA-ESA (European Space Agency) Cassini/Huygens mission in 1997.
Ed Stone, left, talks to reporters. This was at a news conference to announce findings from Voyager 2’s flyby of Uranus in 1986. Credit: NASA/JPL-Caltech
“Ed Stone was a leader who dared mighty things in space. He was a dear friend to all who knew him, and a cherished mentor to me personally,” said Nicola Fox, associate administrator for the Science Mission Directorate at NASA Headquarters in Washington. “Ed took humanity on a planetary tour of our solar system and beyond, sending NASA where no spacecraft had gone before.”
Scientific Contributions
Stone served on nine NASA missions as either principal investigator or a science instrument lead and on five others as a co-investigator. These roles primarily involved studying energetic ions from the Sun and cosmic rays from the galaxy. He had the distinction of being one of the few scientists involved with both the mission that has come closest to the Sun (NASA’s Parker Solar Probe) and the one that has traveled farthest from it (Voyager).
“Ed will be remembered as an energetic leader and scientist who expanded our knowledge about the universe — from the Sun to the planets to distant stars — and sparked our collective imaginations about the mysteries and wonders of deep space,” said Laurie Leshin, JPL director and Caltech vice president. “Ed’s discoveries have fueled exploration of previously unseen corners of our solar system and will inspire future generations to reach new frontiers.”
Achievements and Awards
Among Stone’s many awards, the National Medal of Science from President George H.W. Bush stands out as the most prominent. In 2019 he won the Shaw Prize in Astronomy, with an award of $1.2 million, for his leadership in the Voyager project. As the citation noted, the project “has over the past four decades, transformed our understanding of the four giant planets and the outer solar system, and has now begun to explore interstellar space.”
He was also proud to have a middle school named after him in Burlington, Iowa, as an inspiration to young learners. Stone’s contributions have left an indelible mark on the scientific community and beyond.
Ed Stone, second from left, and other members of the Voyager team pose with a model of the spacecraft in 1977, the year the twin probes launched. Credit: NASA/JPL-Caltech
Legacy
Edward C. Stone’s legacy is a testament to the power of curiosity, perseverance, and the human spirit’s quest for knowledge. His work has inspired countless scientists and space enthusiasts, shaping our understanding of the universe and pushing the boundaries of exploration.
“Thank you, Ed, for everything,” said Nicola Fox. “Your legacy has left a tremendous and profound impact on NASA, the scientific community, and the world.”
Edward C. Stone’s life and career were marked by a relentless pursuit of knowledge and an unwavering dedication to space exploration. His leadership of the Voyager mission, his role as director of NASA’s Jet Propulsion Laboratory, and his numerous contributions to our understanding of the solar system and beyond have left an enduring legacy. Stone’s work not only advanced scientific discovery but also inspired the public and future generations of scientists to look to the stars.
His achievements remind us of the vast potential of human ingenuity and the importance of exploring the unknown. As we remember Edward C. Stone, we celebrate a visionary whose impact on space exploration will be felt for generations to come.
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