Chandra X-ray Observatory

and X-ray emissions. Our study, titled “An Improved Age-Activity Relationship for Cool Stars Older than a Gigayear“, was led by Rachel Booth, a PhD student from the Astrophysics Research Center at Queen’s University Belfast. Our data was gathered using NASA's Chandra X-ray Observatory and ESA's XMM-Newton. NASA's Chandra X-ray Observatory is a telescope specifically built to detect X-ray emissions from regions in the universe which exhibit very high temperatures such as stars. ESA's Chandra X-ray

The program uses the same analysis process that an X-ray astronomer would follow in analyzing the data from a Chandra observation. The download instructions to install the ds9 toolbox on your desktop are located at http://chandra-ed.harvard.edu/install.html . The introduction at http://chandra-ed.harvard.edu/learning_ds9overview.html describes the overview and purpose of the software and gives a short summary of the Chandra mission. The tutorial for using the ds9 software is located at

are to what a pulsar travelling at a good chunk of light speed just did to a disk of matter orbiting a giant star. Bruce Lee said to kick to the moon, but Chandra just captured this pulsar just punting the equivalent of a planet into interstellar space. CHANDRA HAS THE BEST SEAT IN THE HOUSE Astronomers using the Chandra X-Ray Observatory orbiting the Earth witnessed the gigantic star called B1259 take this merciless beating in its home constellation Crux, also known as the Southern Cross.

As most of the ultraviolet radiations are blocked by the Ozone layer, so it was very difficult to study ultraviolet radiations from earth’s surface. In order to better understand the Ultraviolet radiation an observatory was created and sent beyond the Earth’s atmosphere. IUE was the first telescope that used Ultraviolet technology. Its purpose was to explore astronomical objects such as galaxies, comets, asteroids, and stars. It weighed 1,420 lbs. and measured

phase during which the hottest layers closest to the surface of the white dwarf can be observed until the hydrogen content of the accreted material is consumed or ejected. The X-ray and UV evolution of novae during their outbursts has been determined using Swift monitoring observations. Deeper, continuous XMM-Newton and Chandra observations have been taken, guided by the long-term evolution determined by Swift. The time when bright SSS emission becomes visible, the turn-on time of the SSS phase, depends

rainbow halo appears around images. Needs little maintenance. It is more resistant to misalignment than the reflecting telescope Heavier, longer and bulkier than other telescope types Optical Telescopes- Reflecting- Ground Based Example- W.M. Keck Observatory (Hawaii, US) How It Works- Instead of using lenses to gather light, these telescopes use concave, primary mirrors at the

Our sun is halfway through its life cycle and based on the studies of the stars, when it reaches the last stages of its life it will go supernova destroying Earth, but that won’t happen in about 5 billion years. Supernovas are the explosion of a star when it reaches the end of its life. There are two ways a star can go supernova. The first way or a Type I supernova occurs in the Binary system which is when two stars orbit the same point. The two stars are a white dwarf and a red giant. A white

Maggie Barnard 8/25/15 Literary Analysis and Comp. II Mrs. Mikowski Supernovae A supernova is a stellar explosion that occurs at the end of a star’s lifetime. It is one of the largest and most energetic explosions in space (S1). A supernova can briefly outshine an entire galaxy and radiate more energy than our sun will in its lifetime. That is about same brightness of 10 million suns (S2). Supernovae happen about every 50 years in a galaxy about the size of the Milky Way, which could be about every

Cygnus A is a radio galaxy, and one of the strongest radio sources in the sky. It was discovered byGrote Reber in 1939. In 1951, Cygnus A, along with Cassiopeia A, and Puppis A were the first "radio stars" identified with an optical source. Of these, Cygnus A became the first radio galaxy; the other two being nebulae inside the Milky Way.[3] In 1953 Roger Jennison and M K Das Gupta showed it to be a double source.[4] Like all radio galaxies, it contains an active galactic nucleus. Images of the galaxy

plentiful. In 2001, Wendy Freedman and other researchers, using data obtained via the HST, calculated the value of H to 72 + 8 [6]. Working with data collected from the Chandra X-Ray Observatory in 2006, researcher Massimiliano Bonamente and his team derived a value for H of 77.6 +14.9, -12.5 [7]. Most recently at the LIGO observatory, the value for H was calculated to be 70.0 +12.0, -8.0