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fuhersatangod:

astropagan:

Understanding Aura Colors

Wouldn’t it be awesome if our followers would send us which one they think we had?

(Source: , via artistsdontsleep)

distant-traveller:

R136 star cluster
Image credit: Hubble Legacy Archive; Processing by: Steven Marx
spaceplasma:

C/2012 S1 (ISON) is a sungrazing comet discovered on 21 September 2012 by Vitali Nevski and Artyom Novichonok. The comet will come to perihelion (closest approach to the Sun) on 28 November 2013 at a distance of 0.012 AU (1,800,000 km; 1,100,000 mi) from the center point of the Sun.
Between 5 June and 29 August 2013, comet ISON will have an elongation less than 30 degrees from the Sun. The Spitzer Space Telescope may observe the comet on June 13 and help estimate carbon dioxide production. Around September 2013, it should become bright enough to be visible through small telescopes or binoculars. But the comet is not expected to reach the naked eye magnitude of 6 until November.Assuming it survives perihelion passage, it should be visible to the naked eye until early January 2014.
In October, the comet will pass through the constellation Leo, passing near Leo’s brightest star Regulus and then passing near Mars in the night sky, and these brighter objects might make the comet easier to locate. STEREO should be able to view ISON around 10 October. In November, when the comet is brighter, it will sweep past another bright star in our sky, Spica in the constellation Virgo, and another planet, Saturn. SOHO will be able to view ISON starting 27 November. Around the time the comet reaches its perihelion on 28 November, it may become extremely bright if it remains intact, probably reaching a negative magnitude. It may briefly become brighter than the full Moon.
It is expected to be brightest around the time it is closest to the Sun; however, it may be less than 1° from the Sun at its closest, making it difficult to see against the Sun’s glare. In December, the comet will be growing dimmer, but, assuming that it remains intact, it will be visible from both hemispheres of Earth, possibly with a long tail.

abcstarstuff:

Another record-breaking Ariane 5 success for Arianespace: ATV Albert Einstein is on its way to the International Space Station

Preparations at the Spaceport for Arianespace launches are highlighted in these photos.

Top is Flight VA213’s heavy-lift Ariane 5, shown in the ELA-3 launch zone prior to today’s liftoff with ATV Albert Einstein.

The medium-lift Soyuz for Flight VS05 (center photo) receives its third stage inside the ELS launch site’s MIK integration building, while the core cryogenic stage for Ariane 5’s VA215 launcher (lower) is unloaded from a sea-going ship that arrived in French Guiana this week.

Bottom image… Ariane 5 lifts off with its heaviest payload ever – ATV Albert Einstein – at the start of the workhorse vehicle’s 69th launch from French Guiana.

(Source: starstuffblog, via n-a-s-a)

stellar-indulgence:

Ngc 660, Polar Ring Galaxy In Pisces
Credit: Robert Gendler
unstablemonkey:

Columbia and Challenger together
n-a-s-a:

M2-9 (Minkowski Butterfly)
Credit: Josef Pöpsel, Beate Behle
spaceplasma:

A run on Fusor V showing X-rays effecting the CCD
Fusor V: X-ray and Neutron Emissions
The fusor, is an apparatus designed to create nuclear fusion. Unlike most controlled fusion systems, which slowly heat a magnetically confined plasma, the fusor injects high energy ions directly into a reaction chamber, thereby avoiding a considerable amount of complexity. The approach is known as inertial electrostatic confinement (IEC).
Regardless of its possible use as an energy source, the fusor has already been demonstrated as a viable neutron source. Fluxes are not as high as can be obtained from nuclear reactor or particle accelerator sources, but are sufficient for many uses.
Watch the video
Credit: Robert Tubbs
 
spaceplasma:

T Tauri and Hind’s Variable Nebula
The orange star centered in this remarkable telescopic skyview is T Tauri, prototype of the class of T Tauri variable stars. Nearby it is a dusty yellow cosmic cloud historically known as Hind’s Variable Nebula (NGC 1555/1554). Over 400 light-years away, at the edge of a molecular cloud, both star and nebula are seen to vary significantly in brightness but not necessarily at the same time, adding to the mystery of the intriguing region. T Tauri stars are now generally recognized as young (less than a few million years old), sun-like stars still in the early stages of formation. To further complicate the picture, infrared observations indicate that T Tauri itself is part of a multiple system and suggest that the associated Hind’s Nebula may also contain a very young stellar object. The dramatic color image spans about 4 light-years at the estimated distance of T Tauri.
Credit & Copyright:  Don Goldman
stellar-indulgence:

Beyond the Borders of a Galaxy
The outlying regions around the Southern Pinwheel galaxy, or M83, are highlighted in this composite image from NASA’s Galaxy Evolution Explorer and the National Science Foundation’s Very Large Array in New Mexico. The blue and pink pinwheel in the center is the galaxy’s main stellar disk, while the flapping, ribbon-like structures are its extended arms.
The Galaxy Evolution Explorer is an ultraviolet survey telescope. Its observations, shown here in blue and green, highlight the galaxy’s farthest-flung clusters of young stars up to 140,000 light-years from its center. The Very Large Array observations show the radio emission in red. They highlight gaseous hydrogen atoms, or raw ingredients for stars, which make up the lengthy, extended arms.
Astronomers are excited that the clusters of baby stars match up with the extended arms, because this helps them better understand how stars can be created out in the “backwoods” of a galaxy.
In this image, far-ultraviolet light is blue, near-ultraviolet light is green and radio emission at a wavelength of 21 centimeters is red.
What Lies Beyond the Edge of a GalaxyThe side-by-side comparison shows the Southern Pinwheel galaxy, or M83, as seen in ultraviolet light (right) and at both ultraviolet and radio wavelengths (left). While the radio data highlight the galaxy’s long, octopus-like arms stretching far beyond its main spiral disk (red), the ultraviolet data reveal clusters of baby stars (blue) within the extended arms.
The ultraviolet image was taken by NASA’s Galaxy Evolution Explorer between March 15 and May 20, 2007, at scheduled intervals. Back in 2005, the telescope first photographed M83 over a shorter period of time. That picture was the first to reveal far-flung baby stars forming up to 63,000 light-years from the edge of the main spiral disk. This came as a surprise to astronomers because a galaxy’s outer territory typically lacks high densities of star-forming materials.
The newest picture of M83 from the Galaxy Evolution Explorer is shown at the right, and was taken over a longer period of time. In fact, it is one of the “deepest,” or longest-exposure, images of a nearby galaxy in ultraviolet light. This deeper view shows more clusters of stars, as well as stars in the very remote reaches of the galaxy, up to 140,000 light-years away from its core.
The view at the left is a combination of the ultraviolet picture at the right and data taken by the telescopes of the National Science Foundation’s Very Large Array in New Mexico. The radio data, colored here in red, reveal extended galactic arms of gaseous hydrogen atoms, which are raw ingredients for stars. Astronomers are excited that the remote clusters of baby stars match up with the extended arms, because this helps them better understand how stars can be created out in the boondocks of a galaxy.
M83 is located 15 million light-years away in the southern constellation Hydra.
In the Galaxy Evolution Explorer image on the right, near-ultraviolet light (or longer-wavelength ultraviolet light) is colored yellow and far-ultraviolet light is blue. In the combined image at the left, far-ultraviolet light is blue, near-ultraviolet light is green, and the radio emission at a wavelength of 21 centimeters is red.
Image credit: NASA/JPL-Caltech/VLA/MPIA