The Goddard Space Flight Center has a Flickr account showcasing a series of images of our own home planet. Called “Blue Marble,” these spectacular images are the most detailed true-color image of the entire Earth to date. Using a collection of satellite-based observations, scientists and visualizers stitched together months of observations in 2001 of the land surface, oceans, sea ice, and clouds into a seamless, true-color mosaic of every square kilometer (.386 square mile) of our planet. Your tax dollars at work, these images are freely available to educators, scientists, museums, and the public. This record includes preview images and links to full resolution versions up to 21,600 pixels across.
Our blue marble. Credit: NASA
Compare these new images to the original “Blue Marble” photograph, below, taken by the Apollo 17 crew in 1968. The original Blue Marble by Apollo 17.
Smoke and haze linger over Santiago, Chile after the magnitude 8.8 earthquake on Feb. 27, 2010. Credit: NASA
[/caption]
Haze lingered over the metropolitan area of Santiago, Chile, following a magnitude 8.8 earth quake on February 27, 2010. In an image from the Moderate Resolution Imaging Spectroradiometer (MODIS) on NASA’s Terra satellite at 14:25 UTC, black smoke hung over the northern part of the city, while light-colored haze (perhaps pollution and/or dust) covered the southern part of the city and filled a canyon that cuts eastward into the mountains. Below, in an image acquired on February 23, shows the city and surroundings under clear-sky conditions.
The region around Santiago, Chile on Feb. 23, 2010, before the quake. Credit: NASA
Below, a map of topography and water depth of the west coast of South America, which is a subduction zone, where the Nazca Plate is plowing under the South America Plate at an average rate of 80 millimeters (3 inches) per year. Their collision gives rise to the spectacular Andes Mountains as well as to devastating earthquakes. Lighter colors indicate higher elevation on land and shallower depth in the water. Quake locations and magnitudes are indicated by black circles. The topography is based on radar data collected during the Shuttle Radar Topography Mission, which flew onboard Space Shuttle Endeavour in mid-February 2002.
A map showing topography, water depth and earthquake magnitudes. Credit: NASA
Santiago, the capital city of Chile. One day after the Mega earthquake(M8.8) hit the country. We wish the earliest recovery. Credit: Soichi Noguchi
[/caption] Astronaut Soichi Noguchi, (@Astro_Soichi) who has taken full advantage of being able to use Twitter live from the International Space Station, has been sending down a stream of images he has taken of Chile following the magnitude 8.8 earthquake that hit the country early Saturday. Just recently, he posted the above image, taken directly over Santiago. “Santiago, the capital city of Chile. One day after the Mega earthquake(M8.8) hit the country. We wish the earliest recovery,” Noguchi wrote on Twitter. He also took a video of the ISS astronaut’s view as they flew over Chile earlier today, below.
Here’s another image Noguchi took from the ISS, of the coastline of Chile, near Santiago.
Near Santiago, Chile. Coast line. Credit: Soichi Noguchi
And another, near Concepcion, Chile.
Coastline near Concepcion, Chile. Credit: Soichi Noguchi
For more images from space, follow @Astro_Soichi on Twitter.
The final spacecraft in this series of NASA and NOAA’s “GOES” geostationary environmental weather satellites is ready for launch. GOES stands for Geostationary Operational Environmental Satellite, and in evidence that not all acronyms turn out for the best, this latest satellite in the series is GOES-P. But (to quote the Bad Astronomer) this satellite will be a whiz in helping to provide continuous observations of severe weather events on Earth and space weather, too, as well as providing an update to search and rescue capabilities. Once in orbit GOES-P’s name will change to GOES-15. “GOES are the backbone of NOAA’s severe weather forecasts, monitoring fast-changing conditions in the atmosphere that spawn hurricanes, tornadoes, floods and other hazards,” said Steve Kirkner, GOES program manager at NASA’s Goddard Space Flight Center.
Launch is targeted for March 2, during a launch window from 6:19 to 7:19 p.m. EST from Space Launch Complex 37 at the Cape Canaveral Air Force Station on a Delta IV rocket. Universe Today will be on location to provide coverage of all the launch and pre-launch activities. Follow Nancy on Twitter for live updates.
“The latest series of satellites, GOES- N, O, and P has new capabilities in space weather,” said Dr. Howard Singer from NOAA. “This is data that arrives almost instantaneously and therefore allows us to provide very timely alerts and warnings.”
But GOES-P will be a back-up satellite. Once launched, it will be checked out and then stored on-orbit and ready for activation should one of the operational GOES satellites degrade or exhaust their fuel. Currently, NOAA operates GOES-12, (GOES East) and GOES-11 (GOES-West.) In late April, NOAA will activate GOES-13 to replace GOES-12, and move GOES-12 to provide coverage for South America as part of the Global Earth Observing System of Systems (GEOSS). NASA handed over GOES-14, launched last June, to NOAA on December 14, 2009.
In addition to weather forecasting on Earth, a key instrument onboard GOES-P, the Solar X-Ray Imager (SXI), will help NOAA continue monitoring solar conditions.
“The SXI is improving our forecasts and warnings for solar disturbances, protecting billions of dollars worth of commercial and government assets in space and on the ground, and lessening the brunt of power surges for the satellite-based electronics and communications industry,” said Tom Bodgan, director of NOAA’s Space Weather Prediction Center (SWPC) in Boulder, Colo.
GOES P is the last in the series. The first GOES satellite was launched in 1975.
GOES-P joins a system of weather satellites that provide timely environmental information to meteorologists and the public. The GOES system provides data used to graphically display the intensity, path and size of storms. Early warning of impending severe weather enhances the public’s ability to take shelter and protect property.
The ESA has scheduled the launch of Cryosat-2 for February 25th aboard a Russian Dnepr rocket from the Baikonur Cosmodrome in Kazakhstan. This is the second attempt at launching the Earth-observing satellite that’s tasked with monitoring global ice thickness. The initial launch of Cryosat on October 8th, 2005 failed due to an anomaly of the launch sequence.
Other Earth-observing satellites have taken measurements of the ice thickness near the poles, but Cryosat-2 will be the first such satellite completely dedicated to monitoring ice thickness variations, and will keep tabs on the decline of sea ice, which in the Arctic has been shown to have shrunk 2.7% per decade since 1978.
Cryosat-2 will have a highly inclined polar orbit, and will reach 88 degrees north and south, so as to maximize the amount of observations of the Earth’s poles. The instruments aboard the satellite will be able to monitor the thickness changes in both sea ice and land ice with an accuracy of one centimeter. This will give scientists an unprecedented amount of data to work with to study how Arctic and Antarctic ice changes impact climate change, and vice versa.
The instrument aboard Cryosat-2 that will be measuring ice thickness is the SAR/Interferometric Radar Altimeter (SIRAL). This is a an altimeter and interferometer that operates in the Ku-band (13.575 GHz), and uses radar signals bounced off the ice to measure its thickness variations.
Cryosat-2 also has two other instruments to determine its position with a high amount of accuracy, the Doppler Orbit and Radio Positioning Integration by Satellite (DORIS) and Laser Retro-Reflector (LRR). DORIS detects and measures the Doppler shift of signals broadcast from a network of radio beacons spread around the world to give the velocity of the satellite relative to the Earth.
The LRR instrument will complement and help calibrate DORIS. The LRR is a small laser retroreflector that is attached to the underside of the satellite, and lasers from a network of tracking stations will be fired at the satellite. By measuring the interval between the firing of the laser and the return of the pulse, the position of the satellite can be measured very accurately.
The mission has a three-year lifespan, with a potential for a two-year extension. Cryosat-2 is currently nestled safely inside the Dnepr rocket’s protective fairing, and in the next nine days the satellite will be integrated into the rest of the launcher and moved out to the launch pad.
Launch Complex 41: Atlas rocket was rolled from VIF at left to pad at right on Feb 9, 2010. Credit: Ken Kremer
[/caption]
(Editor’s Note: Ken Kremer is at the Kennedy Space Center for Universe Today covering the launch of SDO and Endeavour.)
NASA’s nearly $1 Billion hi tech sun probe, the Solar Dynamics Observatory or SDO, was rolled out today (Feb 9) to Launch Pad 41 on a rainy day here in Florida at 1 day from blast off. SDO will be carried aloft atop an Atlas V rocket at 10:26 AM EST on Feb 10 at Cape Canaveral Air Force Station. The launch window extends for 1 hour. The current weather prediction is only 40% “GO”. The primary concerns for launch day are ground winds with gusts and thick clouds.
NASA’s SDO sun explorer is encapsulated inside 4 meter payload fairing and is bolted atop Centaur Upper Stage of Atlas V rocket at Launch Complex 41. Umbilical lines at right carry cryogenic propellants, electrical power and purge gases. Credit: Ken KremerAt the Kennedy Space Center, I was thrilled to watch the rocket rollout to the pad this morning as part of a NASA Media event along with Universe Today Senior Editor Nancy Atkinson. We were accompanied by a group of SDO managers and science investigators from across the country. The rollout started from inside the 30 story gantry known as the VIF, or Vertical Integration Facility, and ended at the launch pad. It took approximately 35 minutes for the twin “trackmobiles” to push the Atlas rocket about 1800 ft along railroad tracks.
Atlas V booster is 12.5 ft in diameter and 106.5 ft in length. Centaur Upper Stage is 10 ft in diameter and 41.5 ft long. SDO payload fairing is 14 ft in diameter. Total Vehicle height is about 189 ft. Credit: Ken KremerThis afternoon I traveled directly inside the highly restricted security zone which surrounds Launch Complex 41 for a photo shoot to observe the assembled Atlas V rocket and SDO spacecraft directly at the pad. Fantastic experience despite the rainstorm.
SDO, Atlas V and Ken in ditch below rocket less than 24 hours from blast off. Credit: Ken Kremer
SDO project scientist Dean Pesnell told me in an interview today that “SDO will acquire movies of the entire surface of the Sun on a 24/7 basis with 10 times greater resolution than High Definition. That’s about equivalent in size to an IMAX movie”. The three science instruments will collect a staggering 1.5 terabytes of data per day which is equivalent to downloading 500,000 songs. The data will be beamed back continuously to two dedicated ground stations in New Mexico which were specially constructed for SDO. There are no on board recorders due to the huge volume of data.
“It’s perfect timing to launch and study the sun as it starts the rise to a solar maximum,” according to Pesnell. “The sun patiently waited for us to be ready to launch as we waited for a launch opportunity. After a long period of inactivity, Sun spots recently started appearing at the North Pole. And they also just started at the South Pole”.
“SDO was conceived by the scientists around 1996 and formally approved by NASA in 2002”, Prof. Phillip Scherrer said to me. He is the Principal Investigator for the Helioseismic and Magnetic Imager (HMI) instrument.
“The primary mission phase will last 5 years and hopefully extend out to 10 and perhaps even longer. The longevity depends on the health of the science instruments. Remember SOHO was projected to last 2 years and has now operated for over 15 years ! “
HMI will study the origin of solar variability and attempt to characterize and understand the Sun’s interior and magnetic activity.
Both HMI, and the Atmospheric Imaging Assembly, or AIA, will allow scientists to see the entire disc of the sun in very high resolution — 4,096 by 4,096 mm CCDs. In comparison, a standard digital camera uses a 7.176 by 5.329 mm CCD sensor.
AIA also will image the outer layer of the sun’s atmosphere, while the Extreme ultraviolet Variability Experiment, or EVE, measures its ultraviolet spectrum every 10 seconds, 24 hours a day.
We are now less than 12 hours from launch of SDO, NASA’s “New Eye on the Sun”.
Read my earlier SDO reports, including from on site at the KSC launch pads for both SDO and STS 130.
Atlas rocket has been rolled to pad 41 on Feb 8, 2010 and is locked in place surrounded by four lightening masts. Credit: Ken KremerAtlas V rocket begins the 1800 ft rollout from VIF to Pad 41. Credit: Ken Kremer
The big snowfall of February 2010 as seen from space. Credit: MODIS Rapid Response Team at NASA GSFC.
[/caption]
Did you live through what has been called “snowmageddon” or “snowpocalypse?” Here’s a satellite’s-eye view of the exceptionally severe winter storm in the Eastern US that dropped several feet of snow on Feb. 6 and 7. Reports of crashed and abandoned cars and hundreds of cancelled flights were interspersed with stories of massive snowball fights. The huge snowfall may hinder highway traffic into midweek, and hundreds of thousands lost electricity. The image comes from the Moderate Resolution Imaging Spectroradiometer (MODIS) on NASA’s Terra satellite. Snow blankets the area hundreds of kilometers inland from the Atlantic coastline.
False-color composite image of the Port-au-Prince, Haiti region, taken Jan. 27, 2010 by NASA’s UAVSAR airborne radar. The city is denoted by the yellow arrow; the black arrow points to the fault responsible for the Jan. 12 earthquake. Image credit: NASA
[/caption]
A modified NASA Gulfstream III aircraft began a three-week campaign to provide a close-up study of the fault lines in Haiti with radar. This first image, captured on Jan. 27, 2010 is a false-color composite image of the city of Port-au-Prince, Haiti, (near the center of the image) and the surrounding region. This image and subsequent images taken by the Uninhabited Aerial Vehicle Synthetic Aperture Radar (UAVSAR) will be combined to measure the motion of Earth’s surface. The earthquake in Haiti on January 12, 2010 has increased the stress on this fault line, significantly increasing the risk of a future earthquake, according to a recent report by the U.S. Geological Survey.
The UAVSAR uses a technique called interferometry. The polarimetric L-band synthetic aperture radar (SAR) specifically designed to acquire airborne repeat track SAR data for differential interferometric measurements, and these measurements will allow scientists to study the pressures building up and being released on the fault at depth. NASA Grumman Gulfstream III (G-III) in flight with the UAVSAR instrument. Credit: NASA
Shortly before 5 p.m. local time on Jan. 12, 2010, a magnitude 7.0 earthquake struck southern Haiti. The earthquake’s epicenter was about 25 kilometers (15 miles) west-southwest of Port-au-Prince, close to the west (left) edge of this image. The large linear east-west valley in the mountains south of the city is the location of the major active fault zone responsible for the earthquake: the Enriquillo-Plantain Garden fault.
The fault extends from the western tip of Haiti past Port-au-Prince into the Dominican Republic to the east of this image.
Satellite interferometric synthetic aperture radar measurements show that the Jan. 12 earthquake ruptured a segment of the fault extending from the epicenter westward over a length of about 40 kilometers (25 miles), leaving the section of the fault in this image unruptured.
Historical records show that the southern part of Haiti was struck by a series of large earthquakes in the 1700s, and geologists believe those were also caused by ruptures on this fault zone.
The large dark line running east-west near the city is the main airport.
The colors in the image reflect the three different UAVSAR radar polarizations: HH (horizontal transmit, horizontal receive) is colored red; VV (vertical transmit, vertical receive) is colored blue; and HV (horizontal transmit, vertical receive) is colored green. Like a pair of Polaroid sunglasses, these images are sensitive to different parts of the radar signal that is reflected back from Earth’s surface. The HV polarization is sensitive to volume scattering that typically occurs over vegetation—this gives hills a greenish color. VV polarization is sensitive to surface scattering such as that returned from bare surfaces or water—this gives water a bluish tint. Finally, HH polarization is sensitive to corner-like objects—this gives some urban areas and vegetated regions a reddish tint. The image is roughly 20 kilometers (12.5 miles) wide in the northwest-southeast direction. North is up and radar illumination is from the southeast.
Twitpic of Golden Gate Bridge in San Francisco, CA from the ISS on Jan 30, 2010 Credit Astronaut Soichi Noguchi
[/caption]
“Golden Gate Bridge, San Fransisco, CA. Beautiful shadow :-),” tweeted Astronaut Soichi Noguchi along with a live image he shot from space from inside the International Space Station.
The 5 man crew comprising Expedition 22 aboard the ISS now have the capability to transmit live, unfiltered views and comments from space. And whats more is that starting on Feb. 1 they’ll be streaming live video from the outpost, orbiting some 220 miles above the earth while speeding along at 17,500 MPH.
Astronaut TJ Creamer twittered the first unassisted post only 1 week ago on Jan 22.
Yesterday afternoon (Jan 30) he tweeted about his next picture targets, “Gonna try to take some pix of the Moon and the mesospheric clouds.”
“Noctilucent clouds. Antarctic. Priceless.” Credit: Astronaut Soichi NoguchiNoguchi sent down other beautiful shots, including “priceless” noctilucent clouds above Antarctica, city lights above Tokyo, and Port-Au-Prince, Haiti with “prayers” from the crew. He shot these In between his station work.
Noguchi tweeted on Jan 29, that he was working with the Japanese robotic arm (JEMRMS) which is attached to Japan’s giant “Kibo” science research module. “JMSRMS is working just fine-just like sim on the ground. I am very excited. The task is to check the status of external experiment facility. KOOL:-).” Kibo is the largest research laboratory on the ISS.
You can follow all the tweets from three of the crew; Astronauts Soichi Noguchi, TJ. Creamer and Jeff Williams at this link: http://twitter.com/NASA_Astronauts
“Great Saturday on board ISS. Taking photos of Earth, preparing for Shuttle arrival, Station maintenance, and calls home.” Reports Jeff Williams in the newest tweet.
“Our internal cameras wlll stream to the Web beginning Monday [Feb 1] ! Wave when you see us!! :)” tweets Creamer.
The live video will be available during all crew duty hours and when the complex is in contact with the ground through its high-speed communications antenna and NASA’s Tracking and Data Relay Satellite System. Live streaming video of the earth and the stations exterior has been available since March 2009.
Meanwhile, everything remains on schedule for the Feb. 7 launch of STS 130 to deliver the Tranquility and Cupola modules.
Illustration of solar wind impact on Earth's magnetosphere Copyright: NASA
[/caption]
While Earth’s magnetic field protects our planet from most of the permanent flow of particles from the solar wind, rifts or fissures in natural shield are known to occur, enabling the solar wind to penetrate our near-space environment. An ESA satellite cluster called, appropriately, Cluster has provided new insight into the location and duration of these ruptures in the Earth’s magnetic shield, and reveals while our atmosphere protects us for the most part, clear effects of these rifts have been detected high in the upper atmosphere and in the region of space around Earth where satellites orbit.
This study reports the observation of fissures on the Sun-facing side of the Earth’s magnetic shield – the dayside magnetopause. Fortunately, these fissures don’t expose Earth’s surface to the solar wind; our atmosphere protects us. But the upper atmosphere is affected. , clear effects have been detected high in the upper atmosphere and in the region of space around Earth where satellites orbit. Credit: ESA
The dominant physical process causing these cracks is known as magnetic reconnection, a process whereby magnetic field lines from different magnetic domains collide and reconnect: opening the closed magnetic shield. Magnetic reconnection is a physical process at work throughout the Universe, from star formation to solar explosions to experimental fusion reactors on Earth. However, the conditions under which it occurs and how long it lasts remain unclear.
What is known is that magnetic reconnection leads to the mixing of previously separated plasmas when, for instance, the solar wind plasma enters the magnetosphere. In this instance the two magnetic domains are the Earth’s internal magnetic field, and the interplanetary magnetic field (IMF). (The solar wind is not only composed of solar particles (mostly protons and electrons), it also carries the Sun’s magnetic field. Out among the planets, this field is the IMF.)
For more than 700,000 years, the South to North orientation of the terrestrial magnetic field has been rather steady. In contrast, the IMF orientation is highly variable, with total inversion frequently observed on times-scales of minutes.
Reconnection between the IMF and the Earth’s magnetic field critically depends on the angle between these fields. Space physicists have made a distinction between reconnection when both fields are in opposite directions, or anti-parallel, and component reconnection, when the IMF is neither parallel nor anti-parallel to the terrestrial magnetic field. The distinction is important since component and anti-parallel reconnection have different onset characteristics and lead to different duration of the fissures in the magnetic shield. The distinction between these two types of magnetic reconnection has been the subject of hot debate among space scientists for many years. The position, on 25 February 2005, of the Cluster satellite constellation and the Double Star TC-1 satellite with respect to the magnetopause. Blue lines represent magnetic field lines related to the Earth's magnetic field. Spacecraft configurations are scaled by a factor of 5.
For the first time, four spacecraft flying in constellation (the ESA Cluster mission), have provided unambiguous evidence of anti-parallel reconnection at high latitude on the dayside magnetopause, occurring quasi-simultaneously with a period of low-latitude component reconnection detected by the Sino-European Double Star TC-1 satellite. TC-1 and the Cluster array (with the Cluster spacecraft separated by ~2000 km) are more than 30,000 km apart (see below.) The 3D reconnection picture, determined by repeated sampling of the ion diffusion region and associated magnetic null fields (i.e. the heart of the reconnection process). 2.
“These observations support the idea that both anti-parallel and component reconnection occur at the dayside magnetopause under the same IMF conditions and that both phenomena might be the local signatures of a global reconnection picture”, says Professor Malcolm Dunlop from the Rutherford Appleton Laboratory, Didcot, UK.
“This remarkable set of observations shows that magnetic reconnection at the magnetopause is not as simple as it is described in textbooks! It also demonstrates the need for the capability to study magnetic reconnection at multiple scales simultaneously”, says Matt Taylor, acting Cluster project scientist at the European Space Agency.
