
General Relativity and Black Holes
... energetic objects called `qso’s or `quasars’ have been identified a large distances and lookback times. • The only explanation astronomers could come up with for their energy source was accreting mass onto a large (>105Mo) black hole. ...
... energetic objects called `qso’s or `quasars’ have been identified a large distances and lookback times. • The only explanation astronomers could come up with for their energy source was accreting mass onto a large (>105Mo) black hole. ...
SolarDermatology
... cool clouds). Held up by magnetic structures, they can live for weeks/months, and are seen as bright against the black background of space. They can reach heights of several 100,000 km above the limb. They eventually become unstable and erupt. A prominence would be a filament if observed on the disk ...
... cool clouds). Held up by magnetic structures, they can live for weeks/months, and are seen as bright against the black background of space. They can reach heights of several 100,000 km above the limb. They eventually become unstable and erupt. A prominence would be a filament if observed on the disk ...
Chapter 13 Practice Questions
... D) Nuclear reactions during the formation of the universe (the Big Bang) ...
... D) Nuclear reactions during the formation of the universe (the Big Bang) ...
Document
... EGRET detected 66 (+27) sources of this type. New breakthrough is expected after the launch of GLAST. Several sources have been detected in the TeV range by ground-based gamma-ray telescopes. All of them, except M87, are BL Lacs at z<0.2 (more percisely, to high-frequency-peaked BL Lac – HBL). ...
... EGRET detected 66 (+27) sources of this type. New breakthrough is expected after the launch of GLAST. Several sources have been detected in the TeV range by ground-based gamma-ray telescopes. All of them, except M87, are BL Lacs at z<0.2 (more percisely, to high-frequency-peaked BL Lac – HBL). ...
Death of Stars with the Mass of 0.3
... collapsing continues until it is hot enough for heavier elements to fuse. If the red giant has only a mass of less than about 1.4 sun masses, the fusion stops after the helium in the core has been burned up. Due to gravitational pressure, the star gets compressed and becomes a white dwarf. The outer ...
... collapsing continues until it is hot enough for heavier elements to fuse. If the red giant has only a mass of less than about 1.4 sun masses, the fusion stops after the helium in the core has been burned up. Due to gravitational pressure, the star gets compressed and becomes a white dwarf. The outer ...
Stellar Remnants White Dwarfs Neutron Stars
... • The reason is that the mass is so compact that you can get within a few kilometers of a full solar mass of material. Today, if you stood on the surface of the Sun, much of the material is hundreds of thousands of kilometers away. With a black hole, the mass is so concentrated that you can get ver ...
... • The reason is that the mass is so compact that you can get within a few kilometers of a full solar mass of material. Today, if you stood on the surface of the Sun, much of the material is hundreds of thousands of kilometers away. With a black hole, the mass is so concentrated that you can get ver ...
Can we determine the grain composition of the Interstellar Medium with
... Motivation for Dust Studies Gets in the way of everything ...
... Motivation for Dust Studies Gets in the way of everything ...
Radio Bubbles, Cooling X-ray Gas, Galaxy Interactions, and Star
... The X-ray cluster 2A0335+096 (z = 0.035) is a nearby X-ray luminous cluster with a cool core and a central radiative cooling time shorter than a Hubble time. The cluster was first identified optically (Zwicky et al. 1965). Schwartz et al. (1980) confirmed its positional coincidence with an Ariel V X ...
... The X-ray cluster 2A0335+096 (z = 0.035) is a nearby X-ray luminous cluster with a cool core and a central radiative cooling time shorter than a Hubble time. The cluster was first identified optically (Zwicky et al. 1965). Schwartz et al. (1980) confirmed its positional coincidence with an Ariel V X ...
ASTRONOMY AND ASTROPHYSICS
... relating to the composition of cosmic rays, where the abundance of lithium, beryllium and boron relative to those of carbon and oxygen are enhanced by a factor of almost a million compared to their ÔuniversalÕ abundance. This is understood by assuming that cosmic rays are accelerated in the Galaxy, ...
... relating to the composition of cosmic rays, where the abundance of lithium, beryllium and boron relative to those of carbon and oxygen are enhanced by a factor of almost a million compared to their ÔuniversalÕ abundance. This is understood by assuming that cosmic rays are accelerated in the Galaxy, ...
poll_questions
... star is on the main sequence? • Helium fusion requires three nuclei to interact within a very short amount of time • For a given gas temperature, helium nuclei move slower than hydrogen nuclei • Helium nuclei repel each other more strongly than hydrogen nuclei • All of the above ...
... star is on the main sequence? • Helium fusion requires three nuclei to interact within a very short amount of time • For a given gas temperature, helium nuclei move slower than hydrogen nuclei • Helium nuclei repel each other more strongly than hydrogen nuclei • All of the above ...
Summary - X-ray Astronomy Group at ISAS
... Majority of AGN in the universe do not have strong optical lines or bright optical nuclei– XMM and Chandra deep fields Serious difference between optical and x-ray classification schemes (SAX, XMM and Chandra serendipitous sources) X-ray selected AGN evolve very differently than optically selected o ...
... Majority of AGN in the universe do not have strong optical lines or bright optical nuclei– XMM and Chandra deep fields Serious difference between optical and x-ray classification schemes (SAX, XMM and Chandra serendipitous sources) X-ray selected AGN evolve very differently than optically selected o ...
microquasars
... Microquasars have provided insight into: -THE PHYSICS OF RELATIVISTIC JETS FROM BH’s -THE CONNECTION BETWEEN ACCRETION & EJECTION -THE FORMATION OF BLACK HOLES AND NEUTRON STARS: Can stars of >40 Msolar end as neutron stars rather than BHs ? Do BHs of >10 Msolar form promptly rather than in bright S ...
... Microquasars have provided insight into: -THE PHYSICS OF RELATIVISTIC JETS FROM BH’s -THE CONNECTION BETWEEN ACCRETION & EJECTION -THE FORMATION OF BLACK HOLES AND NEUTRON STARS: Can stars of >40 Msolar end as neutron stars rather than BHs ? Do BHs of >10 Msolar form promptly rather than in bright S ...
Modeling High-Mass X-ray Binary Formation in the Chandra Era Tim Linden
... At each step in stellar evolution, calculate if there are important binary interactions, these generally happen on a faster timescale than stellar evolution ...
... At each step in stellar evolution, calculate if there are important binary interactions, these generally happen on a faster timescale than stellar evolution ...
A Dozen Colliding-Wind X-Ray Binaries in the Star - UvA-DARE
... We analyzed archival Chandra X-ray observations of the central portion of the 30 Doradus region in the Large Magellanic Cloud. The image contains 20 X-ray point sources with luminosities between 5 1032 and 2 1035 ergs s1 (0.2–3.5 keV). A dozen sources have bright WN Wolf-Rayet or spectral type ...
... We analyzed archival Chandra X-ray observations of the central portion of the 30 Doradus region in the Large Magellanic Cloud. The image contains 20 X-ray point sources with luminosities between 5 1032 and 2 1035 ergs s1 (0.2–3.5 keV). A dozen sources have bright WN Wolf-Rayet or spectral type ...
type II supernova
... really bad news for the star. The outer layers of the star come raining down onto the core. Somehow this collapse changes into an explosion: a type II supernova. The process by which this happens is still being investigated, but evidently the core collapses to something below its equilibrium radius ...
... really bad news for the star. The outer layers of the star come raining down onto the core. Somehow this collapse changes into an explosion: a type II supernova. The process by which this happens is still being investigated, but evidently the core collapses to something below its equilibrium radius ...
Introduction to Astrophysics, Lecture 13
... how fast they orbit. Except … Stars towards the outer edge of our galaxy (and others) are orbiting much faster than they ought to, perhaps three times as fast. As the velocity v is proportional to the square root of the mass M of the galaxy, this implies that the galaxy is really about ten times mor ...
... how fast they orbit. Except … Stars towards the outer edge of our galaxy (and others) are orbiting much faster than they ought to, perhaps three times as fast. As the velocity v is proportional to the square root of the mass M of the galaxy, this implies that the galaxy is really about ten times mor ...
rastieee
... integration to the QB50 project. EK also thanks Berkant Ecevit, Eray Akyol, Erdem Baş, Şevket Uludağ of Istanbul Technical University who contributed to this project. ...
... integration to the QB50 project. EK also thanks Berkant Ecevit, Eray Akyol, Erdem Baş, Şevket Uludağ of Istanbul Technical University who contributed to this project. ...
Supermassive black holes - University of Texas Astronomy Home
... Can detect the halo of X-rays from orbiting matter, the accretion disk, near the event horizon that will reveal the presence and nature of the black hole. ...
... Can detect the halo of X-rays from orbiting matter, the accretion disk, near the event horizon that will reveal the presence and nature of the black hole. ...
Test - Scioly.org
... E) Process of a collapsing neutron star 38. At which of the following distances would a Type Ia supernova be most useful for determining a cosmological distance? (T7) A) 500 Kpc B) 1 Mpc C) 500 Mpc D) 1000 Mpc E) 1500 Mpc 39. A white dwarf is unable to have a mass greater than how many solar masses? ...
... E) Process of a collapsing neutron star 38. At which of the following distances would a Type Ia supernova be most useful for determining a cosmological distance? (T7) A) 500 Kpc B) 1 Mpc C) 500 Mpc D) 1000 Mpc E) 1500 Mpc 39. A white dwarf is unable to have a mass greater than how many solar masses? ...
Forging the elements
... Evolved stars LOSE about HALF of their MASS through their stellar winds. The winds are mostly made up of hydrogen. Molecules such as H2O (water) and OH (hydroxyl) form in the stellar winds at large distances from the star. Stellar wind ...
... Evolved stars LOSE about HALF of their MASS through their stellar winds. The winds are mostly made up of hydrogen. Molecules such as H2O (water) and OH (hydroxyl) form in the stellar winds at large distances from the star. Stellar wind ...
neutron star.
... — Beams of radiation from a rotating neutron star sweep through space like lighthouse beams, making them appear to pulse. — Observations of these pulses were the first evidence for neutron stars. ...
... — Beams of radiation from a rotating neutron star sweep through space like lighthouse beams, making them appear to pulse. — Observations of these pulses were the first evidence for neutron stars. ...
Monster Black Holes - Indiana University Astronomy
... Evidence for Black Holes Effect of gravity on nearby objects – Mass! Accretion disks Accretion disks emit x-rays as matter falls in But it’s hard to tell the difference between a black hole and a neutron star ...
... Evidence for Black Holes Effect of gravity on nearby objects – Mass! Accretion disks Accretion disks emit x-rays as matter falls in But it’s hard to tell the difference between a black hole and a neutron star ...
Stars and The Universe
... it to heat back up and turn from red to white. 13. Eventually, our sun will turn into a black dwarf. Why? The compression that heats up a white dwarf is the last energy source for the sun. After this energy is radiated into space, there will be no more. The sun will become cold and dark. This stage ...
... it to heat back up and turn from red to white. 13. Eventually, our sun will turn into a black dwarf. Why? The compression that heats up a white dwarf is the last energy source for the sun. After this energy is radiated into space, there will be no more. The sun will become cold and dark. This stage ...
CHP 14
... c. the material will become hot enough that it will radiate most strongly at x-ray wavelengths. d. as the material slows down it converts thermal energy to gravitational potential energy. e. none of the above A rotating black hole a. will produce a pulsar. b. will have a stronger gravitational field ...
... c. the material will become hot enough that it will radiate most strongly at x-ray wavelengths. d. as the material slows down it converts thermal energy to gravitational potential energy. e. none of the above A rotating black hole a. will produce a pulsar. b. will have a stronger gravitational field ...
Neutron Stars and Black Holes
... c. the material will become hot enough that it will radiate most strongly at x-ray wavelengths. d. as the material slows down it converts thermal energy to gravitational potential energy. e. none of the above A rotating black hole a. will produce a pulsar. b. will have a stronger gravitational field ...
... c. the material will become hot enough that it will radiate most strongly at x-ray wavelengths. d. as the material slows down it converts thermal energy to gravitational potential energy. e. none of the above A rotating black hole a. will produce a pulsar. b. will have a stronger gravitational field ...
Astrophysical X-ray source

Astrophysical X-ray sources are astronomical objects with physical properties which result in the emission of X-rays.There are a number of types of astrophysical objects which emit X-rays, from galaxy clusters, through black holes in active galactic nuclei (AGN) to galactic objects such as supernova remnants, stars, and binary stars containing a white dwarf (cataclysmic variable stars and super soft X-ray sources), neutron star or black hole (X-ray binaries). Some solar system bodies emit X-rays, the most notable being the Moon, although most of the X-ray brightness of the Moon arises from reflected solar X-rays. A combination of many unresolved X-ray sources is thought to produce the observed X-ray background. The X-ray continuum can arise from bremsstrahlung, either magnetic or ordinary Coulomb, black-body radiation, synchrotron radiation, inverse Compton scattering of lower-energy photons be relativistic electrons, knock-on collisions of fast protons with atomic electrons, and atomic recombination, with or without additional electron transitions.Furthermore, celestial entities in space are discussed as celestial X-ray sources. The origin of all observed astronomical X-ray sources is in, near to, or associated with a coronal cloud or gas at coronal cloud temperatures for however long or brief a period.