What is the biggest star? - University of Central Lancashire
... The Gemini telescope in Chile was 8 meters in diameter, all the way across. We are not building telescopes that are 30 meters in diameter so imagine what we can see with them! How hot is the biggest star? The biggest star is called R136a1 and is about 10 times hotter than the Sun on the surface, but ...
... The Gemini telescope in Chile was 8 meters in diameter, all the way across. We are not building telescopes that are 30 meters in diameter so imagine what we can see with them! How hot is the biggest star? The biggest star is called R136a1 and is about 10 times hotter than the Sun on the surface, but ...
Seyfert Galaxies - Otterbein University
... The Tully-Fisher Relation • A relation between the rotation speed of a spiral galaxy and its luminosity • The more mass a galaxy has the brighter it is the faster it rotates the wider the spectral lines are • Measuring rotation speed allows us to estimate luminosity; comparing to observed (app ...
... The Tully-Fisher Relation • A relation between the rotation speed of a spiral galaxy and its luminosity • The more mass a galaxy has the brighter it is the faster it rotates the wider the spectral lines are • Measuring rotation speed allows us to estimate luminosity; comparing to observed (app ...
Slide 1
... For a white dwarf with R~ 5x108 cm, M~Msun, and L ~ 6.25x1038 MeV/s 200 nm ≤ ν ≤ ~.1 Å This ranges from the UV to X-Rays! However the disk itself, because of a smaller L will emit at longer wavelengths. ...
... For a white dwarf with R~ 5x108 cm, M~Msun, and L ~ 6.25x1038 MeV/s 200 nm ≤ ν ≤ ~.1 Å This ranges from the UV to X-Rays! However the disk itself, because of a smaller L will emit at longer wavelengths. ...
PoS(EVN 2014)058 - Proceeding of science
... Non-thermal radiation can be used as a highly efficient way to identify binary systems. Stellar non-thermal emission is associated with the interaction of two (or more) stellar winds and can therefore be used to directly detect and count binary systems within a cluster. The multi-frequency ...
... Non-thermal radiation can be used as a highly efficient way to identify binary systems. Stellar non-thermal emission is associated with the interaction of two (or more) stellar winds and can therefore be used to directly detect and count binary systems within a cluster. The multi-frequency ...
Dust and molecular gas in the most distant quasars
... • How the most massive black hole – bulge systems evolve at their early stage. • Can we see active building via massive star formation co-eval with rapid black hole accretion? • Dynamical mass; • Black hole – bulge ratios; ...
... • How the most massive black hole – bulge systems evolve at their early stage. • Can we see active building via massive star formation co-eval with rapid black hole accretion? • Dynamical mass; • Black hole – bulge ratios; ...
black hole
... The core of helium ash cannot generate nuclear energy. Nevertheless, it can grow hotter—because it contracts and converts gravitational energy into thermal energy. The rising temperature heats the unprocessed hydrogen just outside the core—hydrogen that was never previously hot enough to fuse. ...
... The core of helium ash cannot generate nuclear energy. Nevertheless, it can grow hotter—because it contracts and converts gravitational energy into thermal energy. The rising temperature heats the unprocessed hydrogen just outside the core—hydrogen that was never previously hot enough to fuse. ...
Abstract - UChicago High Energy Physics
... We consider massive black hole binary systems and information that can be derived about their population and formation history solely from current and possible future pulsar timing array (PTA) results. We use models of the stochastic gravitational-wave background from circular massive black hole bin ...
... We consider massive black hole binary systems and information that can be derived about their population and formation history solely from current and possible future pulsar timing array (PTA) results. We use models of the stochastic gravitational-wave background from circular massive black hole bin ...
Molecular gas in the host galaxy of a quasar at redshift z 5 6.42
... temperature from CO(3-2) to CO(1-0)10, this leads to MðH 2 Þ ¼ 2:2 £ 1010 M ( for J1148 þ 5251. If the FIR luminosity of J1148 þ 5251 is powered by star formation, the implied star formation rate is 3,000 M ( per year (ref. 9). Comparing this to the molecular gas mass implies a short gas depletion t ...
... temperature from CO(3-2) to CO(1-0)10, this leads to MðH 2 Þ ¼ 2:2 £ 1010 M ( for J1148 þ 5251. If the FIR luminosity of J1148 þ 5251 is powered by star formation, the implied star formation rate is 3,000 M ( per year (ref. 9). Comparing this to the molecular gas mass implies a short gas depletion t ...
Word doc - UC-HiPACC - University of California, Santa Cruz
... visible to the naked eye from the southern hemisphere). But its dark matter mass likely exceeded the mass of all the visible stars in the Milky Way. “When all that dark matter first smacked into the Milky Way like a ghostly belly flop, 80 to 90 percent of it was stripped off,” Purcell explained. “Bu ...
... visible to the naked eye from the southern hemisphere). But its dark matter mass likely exceeded the mass of all the visible stars in the Milky Way. “When all that dark matter first smacked into the Milky Way like a ghostly belly flop, 80 to 90 percent of it was stripped off,” Purcell explained. “Bu ...
"Seeing" Dark Matter
... These particular predictions are powerful, because they do not depend on assumptions about how gravity operates over cosmic distances. Since Zwicky’s original observations, astronomers have found many astronomical objects that demand far more gravity than the observed normal matter and the conventi ...
... These particular predictions are powerful, because they do not depend on assumptions about how gravity operates over cosmic distances. Since Zwicky’s original observations, astronomers have found many astronomical objects that demand far more gravity than the observed normal matter and the conventi ...
Milky Way Galaxy Webquest
... 13. Except for size, how does the supermassive black hole in the center of our galaxy differ from typical black holes? ...
... 13. Except for size, how does the supermassive black hole in the center of our galaxy differ from typical black holes? ...
Full PDF
... Quasars are extremely distant objects in our known universe. They are the furthest objects away from our galaxy that can be seen. Quasars are extremely bright masses of energy and light. The name quasar is actually short for quasi-stellar radio source or quasi-stellar object. They are the brightest ...
... Quasars are extremely distant objects in our known universe. They are the furthest objects away from our galaxy that can be seen. Quasars are extremely bright masses of energy and light. The name quasar is actually short for quasi-stellar radio source or quasi-stellar object. They are the brightest ...
On the possibility of a helium white dwarf donor in the presumed
... Abstract. 2S 0918–549 is a low-mass X-ray binary (LMXB) with a low optical to X-ray flux ratio. Probably it is an ultracompact binary with an orbital period shorter than 60 min. Such binaries cannot harbor hydrogen rich donor stars. As with other (sometimes confirmed) ultracompact LMXBs, 2S 0918–549 ...
... Abstract. 2S 0918–549 is a low-mass X-ray binary (LMXB) with a low optical to X-ray flux ratio. Probably it is an ultracompact binary with an orbital period shorter than 60 min. Such binaries cannot harbor hydrogen rich donor stars. As with other (sometimes confirmed) ultracompact LMXBs, 2S 0918–549 ...
Chapter 25 Galaxies and Dark Matter
... Quasars are all very distant, and the light coming to us from them has probably gone through many interesting regions. We can learn about the intervening space by careful study of quasar spectra. ...
... Quasars are all very distant, and the light coming to us from them has probably gone through many interesting regions. We can learn about the intervening space by careful study of quasar spectra. ...
Galaxy Properties - Tufts Institute of Cosmology
... Irregular and peculiar galaxies • Early studies in the 1980’s ...
... Irregular and peculiar galaxies • Early studies in the 1980’s ...
Dark Matter NS Warsaw
... ▸ Since the dark matter density near the Galactic center is significantly higher than regions near the solar position (where the oldest pulsars have been found) there is a parameter space where dark matter accumulation may solve the missing pulsar problem. ...
... ▸ Since the dark matter density near the Galactic center is significantly higher than regions near the solar position (where the oldest pulsars have been found) there is a parameter space where dark matter accumulation may solve the missing pulsar problem. ...
Astrophysics
... elemental composition; and nonthermal, synchrotron emission from extremely energetic electrons, giving information on the shock acceleration process which is probably responsible for producing galactic cosmic rays. Prof. Ellison studies the acceleration of these particles via the Diffusive Shock Ac ...
... elemental composition; and nonthermal, synchrotron emission from extremely energetic electrons, giving information on the shock acceleration process which is probably responsible for producing galactic cosmic rays. Prof. Ellison studies the acceleration of these particles via the Diffusive Shock Ac ...
Elliptical galaxies
... luminosity (E’s), and compact ellipticals (cE’s), covering a range in absolute magnitudes from MB ~−23 to MB ~−15. ...
... luminosity (E’s), and compact ellipticals (cE’s), covering a range in absolute magnitudes from MB ~−23 to MB ~−15. ...
Galaxy Independent Study Assignment
... and they are classified according to the size of the bulge and the tightness and appearance of the arms. The spiral arms, which wrap around the bulge, contain many young blue stars and lots of gas and dust. Stars in the bulge tend to be older and redder. Yellow stars like our Sun are found throughou ...
... and they are classified according to the size of the bulge and the tightness and appearance of the arms. The spiral arms, which wrap around the bulge, contain many young blue stars and lots of gas and dust. Stars in the bulge tend to be older and redder. Yellow stars like our Sun are found throughou ...
Observational Evidence for Dark Matter Simona Murgia, SLAC-KIPAC XXXIX SLAC Summer Institute
... By exploiting line of sight velocities and proper motion of satellite galaxies can determine the galactic halo mass out to large radii Halo mass within 300 kpc (stat error only): ...
... By exploiting line of sight velocities and proper motion of satellite galaxies can determine the galactic halo mass out to large radii Halo mass within 300 kpc (stat error only): ...
White dwarfs from GAIA: The 7th dimension
... • The white dwarf luminosity function of Gaia is a sensitive probe of the averaged star formation rate • Due to their very short main-sequence lifetimes the shape of the SFR can be reconstructed from the luminosity function of massive white dwarfs • To achieve these goals, we need R~5000 spectroscop ...
... • The white dwarf luminosity function of Gaia is a sensitive probe of the averaged star formation rate • Due to their very short main-sequence lifetimes the shape of the SFR can be reconstructed from the luminosity function of massive white dwarfs • To achieve these goals, we need R~5000 spectroscop ...
Groups of Stars
... Spherical shape Generally older stars Surround the galaxy • Out of galaxy plane ...
... Spherical shape Generally older stars Surround the galaxy • Out of galaxy plane ...
Constraining the Bulk Properties of Dense Matter by Measuring
... testing theories of nuclear matter under high pressure. Neutron stars may exhibit conditions and phenomena not observed elsewhere, such as hyperon-dominated matter, deconfined quark matter, superfluidity and superconductivity with critical temperatures near 1010 kelvin, opaqueness to neutrinos, and ...
... testing theories of nuclear matter under high pressure. Neutron stars may exhibit conditions and phenomena not observed elsewhere, such as hyperon-dominated matter, deconfined quark matter, superfluidity and superconductivity with critical temperatures near 1010 kelvin, opaqueness to neutrinos, and ...
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.