Finalists For A Future Mission To Explore The Solar System

Landslides in Japan

On Sept. 6, 2018, shortly after the remnants of Typhoon Jebi drenched southern Hokkaido, a powerful earthquake rattled the Japanese island. The 6.6-magnitude quake shook the surface enough to unleash hundreds of landslides.

The Landsat 8 satellite acquired imagery of the widespread damage. An image acquired on Sept. 15, 2018, shows mud and debris in a hilly area east of Abira. For comparison, the previous image shows the same area on July 26, 2017.

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Packing for a Journey into the Twilight Zone

Submitted for your consideration: A team of researchers from more than 20 institutions, boarding two research vessels, heading into the ocean’s twilight zone.

The twilight zone is a dimly lit region between 650 and 3300 feet below the surface, where we’re unfolding the mystery of how tiny ocean organisms affect our planet’s climate.

These tiny organisms – called phytoplankton – are plant-like and mostly single-celled. They live in water, taking in carbon dioxide and releasing oxygen.

Two boats, more than 100 researchers from more than 20 partner institutions, and a whole fleet of robotic explorers make up the EXport Processes in the Ocean from RemoTe Sensing (EXPORTS) team. We’re learning more about what happens to carbon dioxide after phytoplankton digest it.

The Equipment to Find Phytoplankton

Phytoplankton have predators in the ocean called zooplankton. They absorb the phytoplankton’s carbon, carrying it up the food chain. The EXPORTS mission will focus partly on how that happens in the ocean’s twilight zone, where some zooplankton live.  When phytoplankton die, sometimes their bodies sink through the same area. All of this carries carbon dioxide into the ocean’s depths and out of Earth’s atmosphere.

Counting Life

Studying the diversity of these organisms is important to better understand what’s happening to the phytoplankton as they die. Researchers from the Virginia Institute of Marine Science are using a very fine mesh net to sample water at various depths throughout the ocean to count various plankton populations.

Researchers from the University of Rhode Island are bringing the tools to sequence the DNA of phytoplankton and zooplankton to help count these organism populations, getting a closer look at what lives below the ocean’s surface.

Science at 500 Feet

Taking measurements at various depths is important, because phytoplankton, like plants, use sunlight to digest carbon dioxide. That means that phytoplankton at different levels in the ocean absorb and digest carbon differently. We’re bringing a Wirewalker, an instrument that glides up and down along a vertical wire to take in water samples all along its 500-foot long tether.

This journey to the twilight zone will take about thirty days, but we’ll be sending back dispatches from the ships. Follow along as we dive into ocean diversity on our Earth Expeditions blog: https://blogs.nasa.gov/earthexpeditions.

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@danizzzxix: Does being in space take a toll on your body?

5 Ways the Moon Landing Changed Life on Earth

When Neil Armstrong took his first steps on the Moon 50 years ago, he famously said “that’s one small step for a man, one giant leap for mankind.” He was referring to the historic milestone of exploring beyond our own planet — but there’s also another way to think about that giant leap: the massive effort to develop technologies to safely reach, walk on the Moon and return home led to countless innovations that have improved life on Earth.

Armstrong took one small step on the lunar surface, but the Moon landing led to a giant leap forward in innovations for humanity.

Here are five examples of technology developed for the Apollo program that we’re still using today:

1. Food Safety Standards

As soon as we started planning to send astronauts into space, we faced the problem of what to feed them — and how to ensure the food was safe to eat. Can you imagine getting food poisoning on a spacecraft, hundreds of thousands of miles from home?

We teamed up with a familiar name in food production: the Pillsbury Company. The company soon realized that existing quality control methods were lacking. There was no way to be certain, without extensive testing that destroyed the sample, that the food was free of bacteria and toxins.

Pillsbury revamped its entire food-safety process, creating what became the Hazard Analysis and Critical Control Point system. Its aim was to prevent food safety problems from occurring, rather than catch them after the fact. They managed this by analyzing and controlling every link in the chain, from the raw materials to the processing equipment to the people handling the food.

Today, this is one of the space program’s most far-reaching spinoffs. Beyond keeping the astronaut food supply safe, the Hazard Analysis and Critical Point system has also been adopted around the world — and likely reduced the risk of bacteria and toxins in your local grocery store. 

2. Digital Controls for Air and Spacecraft

The Apollo spacecraft was revolutionary for many reasons. Did you know it was the first vehicle to be controlled by a digital computer? Instead of pushrods and cables that pilots manually adjusted to manipulate the spacecraft, Apollo’s computer sent signals to actuators at the flick of a switch.

Besides being physically lighter and less cumbersome, the switch to a digital control system enabled storing large quantities of data and programming maneuvers with complex software.

Before Apollo, there were no digital computers to control airplanes either. Working together with the Navy and Draper Laboratory, we adapted the Apollo digital flight computer to work on airplanes. Today, whatever airline you might be flying, the pilot is controlling it digitally, based on the technology first developed for the flight to the Moon.

3. Earthquake-ready Shock Absorbers

A shock absorber descended from Apollo-era dampers and computers saves lives by stabilizing buildings during earthquakes.

Apollo’s Saturn V rockets had to stay connected to the fueling tubes on the launchpad up to the very last second. That presented a challenge: how to safely move those tubes out of the way once liftoff began. Given how fast they were moving, how could we ensure they wouldn’t bounce back and smash into the vehicle?

We contracted with Taylor Devices, Inc. to develop dampers to cushion the shock, forcing the company to push conventional shock isolation technology to the limit.

Shortly after, we went back to the company for a hydraulics-based high-speed computer. For that challenge, the company came up with fluidic dampers—filled with compressible fluid—that worked even better. We later applied the same technology on the Space Shuttle’s launchpad.

The company has since adapted these fluidic dampers for buildings and bridges to help them survive earthquakes. Today, they are successfully protecting structures in some of the most quake-prone areas of the world, including Tokyo, San Francisco and Taiwan.

4. Insulation for Space

We’ve all seen runners draped in silvery “space blankets” at the end of marathons, but did you know the material, called radiant barrier insulation, was actually created for space?

Temperatures outside of Earth’s atmosphere can fluctuate widely, from hundreds of degrees below to hundreds above zero. To better protect our astronauts, during the Apollo program we invented a new kind of effective, lightweight insulation.

We developed a method of coating mylar with a thin layer of vaporized metal particles. The resulting material had the look and weight of thin cellophane packaging, but was extremely reflective—and pound-for-pound, better than anything else available.

Today the material is still used to protect astronauts, as well as sensitive electronics, in nearly all of our missions. But it has also found countless uses on the ground, from space blankets for athletes to energy-saving insulation for buildings. It also protects essential components of MRI machines used in medicine and much, much more.

Image courtesy of the U.S. Marines

5. Healthcare Monitors

Patients in hospitals are hooked up to sensors that send important health data to the nurse’s station and beyond — which means when an alarm goes off, the right people come running to help.

This technology saves lives every day. But before it reached the ICU, it was invented for something even more extraordinary: sending health data from space down to Earth.

When the Apollo astronauts flew to the Moon, they were hooked up to a system of sensors that sent real-time information on their blood pressure, body temperature, heart rate and more to a team on the ground.

The system was developed for us by Spacelabs Healthcare, which quickly adapted it for hospital monitoring. The company now has telemetric monitoring equipment in nearly every hospital around the world, and it is expanding further, so at-risk patients and their doctors can keep track of their health even outside the hospital.

Only a few people have ever walked on the Moon, but the benefits of the Apollo program for the rest of us continue to ripple widely.

In the years since, we have continued to create innovations that have saved lives, helped the environment, and advanced all kinds of technology.

Now we’re going forward to the Moon with the Artemis program and on to Mars — and building ever more cutting-edge technologies to get us there. As with the many spinoffs from the Apollo era, these innovations will transform our lives for generations to come.

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The Stellar Buddy System

Our Sun has an entourage of planets, moons, and smaller objects to keep it company as it traverses the galaxy. But it’s still lonely compared to many of the other stars out there, which often come in pairs. These cosmic couples, called binary stars, are very important in astronomy because they can easily reveal things that are much harder to learn from stars that are on their own. And some of them could even host habitable planets!

The birth of a stellar duo

New stars emerge from swirling clouds of gas and dust that are peppered throughout the galaxy. Scientists still aren’t sure about all the details, but turbulence deep within these clouds may give rise to knots that are denser than their surroundings. The knots have stronger gravity, so they can pull in more material and the cloud may begin to collapse.

The material at the center heats up. Known as a protostar, it is this hot core that will one day become a star. Sometimes these spinning clouds of collapsing gas and dust may break up into two, three, or even more blobs that eventually become stars. That would explain why the majority of the stars in the Milky Way are born with at least one sibling.

Seeing stars

We can’t always tell if we’re looking at binary stars using just our eyes. They’re often so close together in the sky that we see them as a single star. For example, Sirius, the brightest star we can see at night, is actually a binary system (see if you can spot both stars in the photo above). But no one knew that until the 1800s.

Precise observations showed that Sirius was swaying back and forth like it was at a middle school dance. In 1862, astronomer Alvan Graham Clark used a telescope to see that Sirius is actually two stars that orbit each other.

But even through our most powerful telescopes, some binary systems still masquerade as a single star. Fortunately there are a couple of tricks we can use to spot these pairs too.

Since binary stars orbit each other, there’s a chance that we’ll see some stars moving toward and away from us as they go around each other. We just need to have an edge-on view of their orbits. Astronomers can detect this movement because it changes the color of the star’s light – a phenomenon known as the Doppler effect.

Stars we can find this way are called spectroscopic binaries because we have to look at their spectra, which are basically charts or graphs that show the intensity of light being emitted over a range of energies. We can spot these star pairs because light travels in waves. When a star moves toward us, the waves of its light arrive closer together, which makes its light bluer. When a star moves away, the waves are lengthened, reddening its light.

Sometimes we can see binary stars when one of the stars moves in front of the other. Astronomers find these systems, called eclipsing binaries, by measuring the amount of light coming from stars over time. We receive less light than usual when the stars pass in front of each other, because the one in front will block some of the farther star’s light.

Sibling rivalry

Twin stars don’t always get along with each other – their relationship may be explosive! Type Ia supernovae happen in some binary systems in which a white dwarf – the small, hot core left over when a Sun-like star runs out of fuel and ejects its outer layers – is stealing material away from its companion star. This results in a runaway reaction that ultimately detonates the thieving star. The same type of explosion may also happen when two white dwarfs spiral toward each other and collide. Yikes!

Scientists know how to determine how bright these explosions should truly be at their peak, making Type Ia supernovae so-called standard candles. That means astronomers can determine how far away they are by seeing how bright they look from Earth. The farther they are, the dimmer they appear. Astronomers can also look at the wavelengths of light coming from the supernovae to find out how fast the dying stars are moving away from us.

Studying these supernovae led to the discovery that the expansion of the universe is speeding up. Our Nancy Grace Roman Space Telescope will scan the skies for these exploding stars when it launches in the mid-2020s to help us figure out what’s causing the expansion to accelerate – a mystery known as dark energy.

Spilling stellar secrets

Astronomers like finding binary systems because it’s a lot easier to learn more about stars that are in pairs than ones that are on their own. That’s because the stars affect each other in ways we can measure. For example, by paying attention to how the stars orbit each other, we can determine how massive they are. Since heavier stars burn hotter and use up their fuel more quickly than lighter ones, knowing a star’s mass reveals other interesting things too.

By studying how the light changes in eclipsing binaries when the stars cross in front of each other, we can learn even more! We can figure out their sizes, masses, how fast they’re each spinning, how hot they are, and even how far away they are. All of that helps us understand more about the universe.

Tatooine worlds

Thanks to observatories such as our Kepler Space Telescope, we know that worlds like Luke Skywalker’s home planet Tatooine in “Star Wars” exist in real life. And if a planet orbits at the right distance from the two stars, it could even be habitable (and stay that way for a long time).

In 2019, our Transiting Exoplanet Survey Satellite (TESS) found a planet, known as TOI-1338 b, orbiting a pair of stars. These worlds are tricker to find than planets with only one host star, but TESS is expected to find several more!

Want to learn more about the relationships between stellar couples? Check out this Tumblr post: https://nasa.tumblr.com/post/190824389279/cosmic-couples-and-devastating-breakups

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How visible will the stars be compared to a normal night sky if I'm in the path of totality? (Sun completely covered)

I’m not entirely sure, but you will be able to see some stars that you normally wouldn’t see. https://eclipse2017.nasa.gov/sites/default/files/publications/Eclipse_brochure-bookmark_508.pdf In fact, during the 1919 eclipse, Sir Arthur Eddington and others used our ability to see stars close to the Sun during the eclipse to help confirm Einstines’ theory of general relativity. https://eclipse2017.nasa.gov/testing-general-relativity

Eclipse 2017 From Space

On Aug. 21, 2017, a total solar eclipse passed over North America. People throughout the continent captured incredible images of this celestial phenomenon. We and our partner agencies had a unique vantage point on the eclipse from space. Here are a few highlights from our fleet of satellites that observe the Sun, the Moon and Earth.

Our Solar Dynamics Observatory, or SDO, which watches the Sun nearly 24/7 from its orbit 3,000 miles above Earth, saw a partial eclipse on Aug. 21.

SDO sees the Moon cross in front of the Sun several times a year. However, these lunar transits don’t usually correspond to an eclipse here on Earth, and an eclipse on the ground doesn’t guarantee that SDO will see anything out of the ordinary. In this case, on Aug. 21, SDO did see the Moon briefly pass in front of the Sun at the same time that the Moon’s shadow passed over the eastern United States. From its view in space, SDO only saw 14 percent of the Sun blocked by the Moon, while most U.S. residents saw 60 percent blockage or more.

Six people saw the eclipse from the International Space Station. Viewing the eclipse from orbit were NASA’s Randy Bresnik, Jack Fischer and Peggy Whitson, the European Space Agency’s Paolo Nespoli, and Roscosmos’ Commander Fyodor Yurchikhin and Sergey Ryazanskiy. The space station crossed the path of the eclipse three times as it orbited above the continental United States at an altitude of 250 miles.

From a million miles out in space, our Earth Polychromatic Imaging Camera, or EPIC, instrument captured 12 natural color images of the Moon’s shadow crossing over North America. EPIC is aboard NOAA’s Deep Space Climate Observatory, or DSCOVR, where it photographs the full sunlit side of Earth every day, giving it a unique view of the shadow from total solar eclipses. EPIC normally takes about 20 to 22 images of Earth per day, so this animation appears to speed up the progression of the eclipse.

A ground-based image of the total solar eclipse – which looks like a gray ring – is superimposed over a red-toned image of the Sun’s atmosphere, called the corona. This view of the corona was captured by the European Space Agency and our Solar and Heliospheric Observatory, or SOHO. At center is an orange-toned image of the Sun’s surface as seen by our Solar Dynamics Observatory in extreme ultraviolet wavelengths of light.

During a total solar eclipse, ground-based telescopes can observe the lowest part of the solar corona in a way that can’t be done at any other time, as the Sun’s dim corona is normally obscured by the Sun’s bright light. The structure in the ground-based corona image — defined by giant magnetic fields sweeping out from the Sun’s surface — can clearly be seen extending into the outer image from the space-based telescope. The more scientists understand about the lower corona, the more they can understand what causes the constant outward stream of material called the solar wind, as well as occasional giant eruptions called coronal mass ejections.

As millions of Americans watched the total solar eclipse that crossed the continental United States, the international Hinode solar observation satellite captured its own images of the awe-inspiring natural phenomenon. The images were taken with Hinode's X-ray telescope, or XRT, as it flew above the Pacific Ocean, off the west coast of the United States, at an altitude of approximately 422 miles. Hinode is a joint endeavor by the Japan Aerospace Exploration Agency, the National Astronomical Observatory of Japan, the European Space Agency, the United Kingdom Space Agency and NASA.

During the total solar eclipse our Lunar Reconnaissance Orbiter, or LRO, in orbit around the Moon, turned one of its instruments towards Earth to capture an image of the Moon’s shadow over a large region of the United States.

As LRO crossed the lunar south pole heading north at 3,579 mph, the shadow of the Moon was racing across the United States at 1,500 mph. A few minutes later, LRO began a slow 180-degree turn to look back at Earth, capturing an image of the eclipse very near the location where totality lasted the longest. The spacecraft’s Narrow Angle Camera began scanning Earth at 2:25:30 p.m. EDT and completed the image 18 seconds later.

Sensors on the polar-orbiting Terra and Suomi NPP satellites gathered data and imagery in swaths thousands of miles wide. The Moderate Resolution Imaging Spectroradiometer, or MODIS, sensor on Terra and Visible Infrared Imaging Radiometer Suite, or VIIRS, on Suomi NPP captured the data used to make this animation that alternates between two mosaics. Each mosaic is made with data from different overpasses that was collected at different times.

This full-disk geocolor image from NOAA/NASA’s GOES-16 shows the shadow of the Moon covering a large portion of the northwestern U.S. during the eclipse.

Our Interface Region Imaging Spectrograph, or IRIS, mission captured this view of the Moon passing in front of the Sun on Aug. 21.  

Check out nasa.gov/eclipse to learn more about the Aug. 21, 2017, eclipse along with future eclipses, and follow us on Twitter for more satellite images like these: @NASASun, @NASAMoon, and @NASAEarth.

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Cracking Earth’s Carbon Puzzle

It’s a scientific conundrum with huge implications for our future: How will our planet react to increasing levels of carbon dioxide in the atmosphere?

Carbon – an essential building block for life – does not stay in one place or take only one form. Carbon, both from natural and human-caused sources, moves within and among the atmosphere, ocean and land. 

We’ve been a trailblazer in using space-based and airborne sensors to observe and quantify carbon in the atmosphere and throughout the land and ocean, working with many U.S. and international partners.

Our Orbiting Carbon Observatory-2 (OCO-2) is making unprecedented, accurate global measurements of carbon dioxide levels in the atmosphere and providing unique information on associated natural processes.

ABoVE, our multi-year field campaign in Alaska and Canada is investigating how changes in Arctic ecosystems such as boreal forests in a warming climate result in changes to the balance of carbon moving between the atmosphere and land.

This August we’re embarking on an ocean expedition with the National Science Foundation to the northeast Pacific called EXPORTS that will help scientists develop the capability to better predict how carbon in the ocean moves, which could change as Earth’s climate changes. 

ECOSTRESS is slated to launch this summer to the International Space Station to make the first-ever measurements of plant water use and vegetation stress on land – providing key insights into how plants link Earth’s global carbon cycle with its water cycle.

Later this year, ECOSTRESS will be joined on the space station by GEDI, which will use a space borne laser to help estimate how much carbon is locked in forests and how that quantity changes over time.

In early 2019, the OCO-3 instrument is scheduled to launch to the space station to complement OCO-2 observations and allow scientists to probe the daily cycle of carbon dioxide exchange processes over much of the Earth.

And still in the early stages of development is the Geostationary Carbon Cycle Observatory (GeoCarb) satellite, planned to launch in the early 2020s. GeoCarb will collect 10 million observations a day of carbon dioxide, methane and carbon monoxide.

Our emphasis on carbon cycle science and the development of new carbon-monitoring tools is expected to remain a top priority for years to come. READ MORE.

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Solar System: 5 Things to Know This Week

Our solar system is huge, so let us break it down for you. Here are 5 things to know this week:

1. It’s Lunacy, Whether by Day or Night

What’s Up in the night sky during November? See all the phases of the moon by day and by night, and learn how to look for the Apollo landing sites. Just after sunset on November 13 and 14, look near the setting sun in the western sky to see the moon as a slender crescent. For more, catch the latest edition of the monthly “What’s Up” Tumblr breakdown.

2. Answer to Longstanding Mars Mystery is Blowin’  in the Wind

What transformed Mars from a warm and wet environment, one that might have supported surface life, to the cold, arid planet it is today? Data from our Mars Atmosphere and Volatile Evolution (MAVEN) mission pins much of the blame on the sun. Streams of charged solar particles crash against the Martian atmosphere, and without much of a magnetic field there to deflect the onslaught, over time the solar wind has stripped the air away.

3. Orbital Maneuvers in the Dark

The New Horizons mission team has set a new record. They recently performed the last in a series of trajectory changes that set the spacecraft on a course for an encounter with a Kuiper Belt object in January 2019. The Kuiper Belt consists of small bodies that orbit the sun a billion miles or more beyond Pluto. These latest course maneuvers were the most distant trajectory corrections ever performed by any spacecraft.

4. Visit Venus (But Not Really — You’d Fry)

Mars isn’t the only available destination. You can visit all the planets, moons and small worlds of the solar system anytime, right from your computer or handheld device. Just peruse our planets page, where you’ll find everything from basic facts about each body to the latest pictures and discoveries. Visit Venus HERE.

5. Titan Then and Now

Nov. 12 marks the 35th anniversary of Voyager 1’s Saturn flyby in 1980. Voyager saw Saturn’s enshrouded, planet-sized moon Titan as a featureless ball. In recent years, the Cassini mission haas revealed Titan in detail as a complex world. The spacecraft has peered beneath its clouds, and even delivered a probe to its encounter, which will include infrared scans, as well as using visible light cameras to look for methane clouds in the atmosphere.

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Three Ways to Travel at (Nearly) the Speed of Light

One hundred years ago, Einstein’s theory of general relativity was supported by the results of a solar eclipse experiment. Even before that, Einstein had developed the theory of special relativity — a way of understanding how light travels through space.

Particles of light — photons — travel through a vacuum at a constant pace of more than 670 million miles per hour.

All across space, from black holes to our near-Earth environment, particles are being accelerated to incredible speeds — some even reaching 99.9% the speed of light! By studying these super fast particles, we can learn more about our galactic neighborhood. 

Here are three ways particles can accelerate:

1) Electromagnetic Fields!

Electromagnetic fields are the same forces that keep magnets on your fridge! The two components — electric and magnetic fields — work together to whisk particles at super fast speeds throughout the universe. In the right conditions, electromagnetic fields can accelerate particles at near-light-speed.

We can harness electric fields to accelerate particles to similar speeds on Earth! Particle accelerators, like the Large Hadron Collider and Fermilab, use pulsed electromagnetic fields to smash together particles and produce collisions with immense amounts of energy. These experiments help scientists understand the Big Bang and how it shaped the universe!

2) Magnetic Explosions!

Magnetic fields are everywhere in space, encircling Earth and spanning the solar system. When these magnetic fields run into each other, they can become tangled. When the tension between the crossed lines becomes too great, the lines explosively snap and realign in a process known as magnetic reconnection. Scientists suspect this is one way that particles — for example, the solar wind, which is the constant stream of charged particles from the Sun — are sped up to super fast speeds.

When magnetic reconnection occurs on the side of Earth facing away from the Sun, the particles can be hurled into Earth’s upper atmosphere where they spark the auroras.

3) Wave-Particle Interactions!

Particles can be accelerated by interactions with electromagnetic waves, called wave-particle interactions. When electromagnetic waves collide, their fields can become compressed. Charged particles bounce back and forth between the waves, like a ball bouncing between two merging walls. These types of interactions are constantly occurring in near-Earth space and are responsible for damaging electronics on spacecraft and satellites in space.

Wave-particle interactions might also be responsible for accelerating some cosmic rays from outside our solar system. After a supernova explosion, a hot, dense shell of compressed gas called a blast wave is ejected away from the stellar core. Wave-particle interactions in these bubbles can launch high-energy cosmic rays at 99.6% the speed of light.

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