DoAr21_AAS2005 - Astronomy at Swarthmore College
... Oph star forming cloud, is a Weak-lined T Tauri Star (WTTS), having shown H-alpha in emission in the 1950s but without H-alpha emission reported subsequently and without a strong IR excess. It is only about 1 Myr old (left) and has already been identified, via lowresolution x-ray spectroscopy, to ha ...
... Oph star forming cloud, is a Weak-lined T Tauri Star (WTTS), having shown H-alpha in emission in the 1950s but without H-alpha emission reported subsequently and without a strong IR excess. It is only about 1 Myr old (left) and has already been identified, via lowresolution x-ray spectroscopy, to ha ...
Slides from Dr. Frank`s Lecture17
... Interacting Binary Stars Why some binaries interact and others don’t? The following processes are inevitable in a binary: 1) The binary separation decreases because of gravitational radiation and other angular momentum losses. 2) The component stars will evolve and change size (for example becomin ...
... Interacting Binary Stars Why some binaries interact and others don’t? The following processes are inevitable in a binary: 1) The binary separation decreases because of gravitational radiation and other angular momentum losses. 2) The component stars will evolve and change size (for example becomin ...
X-ray astronomy - University of Warwick
... and interstellar absorption of NH=1020cm-2, estimate the 2-10 keV energy flux of SU UMa • Further calculate the XMM-Newton RGS count rate, and determine how long an observation is required to accumulate 20,000 RGS counts ...
... and interstellar absorption of NH=1020cm-2, estimate the 2-10 keV energy flux of SU UMa • Further calculate the XMM-Newton RGS count rate, and determine how long an observation is required to accumulate 20,000 RGS counts ...
An approach to ground based space surveillance
... relative distance between the two objects in OOS proximity flight is generally less than 500 m ( 2.5 arcsec as observed from Earth's surface). Some key impediments prevent OOS activities from being detected; (1) the inherent point spread function of the optics and pixel pitch of the detector array ...
... relative distance between the two objects in OOS proximity flight is generally less than 500 m ( 2.5 arcsec as observed from Earth's surface). Some key impediments prevent OOS activities from being detected; (1) the inherent point spread function of the optics and pixel pitch of the detector array ...
High Resolution Imaging of Satellites with Ground-Based
... if these images were acquired in the visible, they are chosen here for K-band images for the sake of the simulation. Flux were calibrated so that the brightest part of each object gets twice the estimated 170 photons per λ/D value so that the average brightness be close to our prediction. Since the ...
... if these images were acquired in the visible, they are chosen here for K-band images for the sake of the simulation. Flux were calibrated so that the brightest part of each object gets twice the estimated 170 photons per λ/D value so that the average brightness be close to our prediction. Since the ...
Watching Galaxies Form Near the Beginning of Time
... The Cosmic Time Machine The finite speed of light means that we always see things after they have happened–a delay of 8 minutes for the Sun and about 12 billion years for the most distant galaxies we can observe. In other words, ...
... The Cosmic Time Machine The finite speed of light means that we always see things after they have happened–a delay of 8 minutes for the Sun and about 12 billion years for the most distant galaxies we can observe. In other words, ...
Supernova Neutrinos
... [*] Astronomy with a Neutrino Telescope and Abyss Environmental RESearch ...
... [*] Astronomy with a Neutrino Telescope and Abyss Environmental RESearch ...
Core-collapse supernovae and their massive progenitors
... II-P SNe that have distinctly lower luminosities and kinetic energies (measured by the expansion velocity of the ejecta) than normal (Pastorello et al. 2004). Explosion models of 8–9 M⊙ stars have been made by Kitaura et al. (2006) in which electron capture by an oxygen–neon–magnesium core triggers ...
... II-P SNe that have distinctly lower luminosities and kinetic energies (measured by the expansion velocity of the ejecta) than normal (Pastorello et al. 2004). Explosion models of 8–9 M⊙ stars have been made by Kitaura et al. (2006) in which electron capture by an oxygen–neon–magnesium core triggers ...
Y-band Imaging of Extragalatic Fields and High redshift
... We carried out the observations of several extragalactic fields, brown dwarfs, high-z QSO and A0V standard star imaging with Y-band filter at the Mt. Lemmon Opti cal Astronomy Observatory (LOAO) and the Maidanak Observatory. The deepest limit magnitude of 260 minutes exposure is Y = 21.5 AB mag in c ...
... We carried out the observations of several extragalactic fields, brown dwarfs, high-z QSO and A0V standard star imaging with Y-band filter at the Mt. Lemmon Opti cal Astronomy Observatory (LOAO) and the Maidanak Observatory. The deepest limit magnitude of 260 minutes exposure is Y = 21.5 AB mag in c ...
nasafinal - University of Oregon
... (hereafter XUV) features around normal galaxies that stimulated our interest in using PMO to discover possible new candidates for follow-up imaging with the GALEX satellite. Using the initial research money granted by the OSGC, we were able to successfully acquire observing time during cycle 4 of th ...
... (hereafter XUV) features around normal galaxies that stimulated our interest in using PMO to discover possible new candidates for follow-up imaging with the GALEX satellite. Using the initial research money granted by the OSGC, we were able to successfully acquire observing time during cycle 4 of th ...
A Chandra Observation of the Massive Star-Forming
... V. X-ray Emission from Massive Stars X-ray emission detected from all OB stars earlier than B1. The brightest source is WR 93 Lx/Lbol~10-7 for the O stars Candidate O stars were found using X-ray luminosity, constant lightcurves, and near IR colors ...
... V. X-ray Emission from Massive Stars X-ray emission detected from all OB stars earlier than B1. The brightest source is WR 93 Lx/Lbol~10-7 for the O stars Candidate O stars were found using X-ray luminosity, constant lightcurves, and near IR colors ...
3. Cosmology and the Origin and Evolution of Galaxies
... peaks at ~ 250 µm and contributes approximately 50% of the total radioX-ray extragalactic background light, and hence it is clearly a component that needs to be spatially resolved and understood. It is also important to note that << 1 square degree of the extragalactic sky has been mapped at mm wave ...
... peaks at ~ 250 µm and contributes approximately 50% of the total radioX-ray extragalactic background light, and hence it is clearly a component that needs to be spatially resolved and understood. It is also important to note that << 1 square degree of the extragalactic sky has been mapped at mm wave ...
Chapter 13
... originate on neutron stars that have binary partners. The process is very similar to a nova, but much more energy is emitted due to the extremely strong gravitational field of the neutron star. ...
... originate on neutron stars that have binary partners. The process is very similar to a nova, but much more energy is emitted due to the extremely strong gravitational field of the neutron star. ...
Chapter 14
... Model of the X-Ray Binary SS 433 Optical spectrum shows spectral lines from material in the jet. Two sets of lines: one blue-shifted, one red-shifted ...
... Model of the X-Ray Binary SS 433 Optical spectrum shows spectral lines from material in the jet. Two sets of lines: one blue-shifted, one red-shifted ...
margarita2007
... the heat radiation of the Big Bang and the large scale distribution of galaxies. ...
... the heat radiation of the Big Bang and the large scale distribution of galaxies. ...
Review: How does a star`s mass determine its life story?
... One famous X-ray binary with a likely black hole is in the constellation Cygnus. ...
... One famous X-ray binary with a likely black hole is in the constellation Cygnus. ...
chapter18StarDeath
... – A black hole is a massive object whose radius is so small that the escape velocity exceeds the speed of light ...
... – A black hole is a massive object whose radius is so small that the escape velocity exceeds the speed of light ...
Chapter 18 The Bizarre Stellar Graveyard What is a white dwarf
... Our goals for learning What is a neutron star? How were neutron stars discovered? What can happen to a neutron star in a close ...
... Our goals for learning What is a neutron star? How were neutron stars discovered? What can happen to a neutron star in a close ...
Chapter 14 Neutron Stars and Black holes
... Model of the X-Ray Binary SS 433 Optical spectrum shows spectral lines from material in the jet. Two sets of lines: one blue-shifted, one red-shifted ...
... Model of the X-Ray Binary SS 433 Optical spectrum shows spectral lines from material in the jet. Two sets of lines: one blue-shifted, one red-shifted ...
Paper - Astrophysics - University of Oxford
... 2.1. Formation of stars across the Universe When did stars form? To answer this basic question we can make use of the fact that every star must eventually die. Indeed the more massive stars die in spectacular supernova explosions that can outshine a whole galaxy. With an ELT these explosions can be ...
... 2.1. Formation of stars across the Universe When did stars form? To answer this basic question we can make use of the fact that every star must eventually die. Indeed the more massive stars die in spectacular supernova explosions that can outshine a whole galaxy. With an ELT these explosions can be ...
Neutron Star
... Black Holes: Accreted matter disappears beyond the event horizon without a trace. ...
... Black Holes: Accreted matter disappears beyond the event horizon without a trace. ...
The Milky Way - National Tsing Hua University
... Black Holes: Accreted matter disappears beyond the event horizon without a trace. ...
... Black Holes: Accreted matter disappears beyond the event horizon without a trace. ...
SARA Beginner Booklet - Society of Amateur Radio Astronomers
... radio voice transmissions at “short wavelengths” (wavelengths of about 10-20 meters). These wavelengths were being considered for transatlantic radio telephones. After recording signals from all directions for several months, Jansky identified three types of static: • nearby thunderstorms • distant ...
... radio voice transmissions at “short wavelengths” (wavelengths of about 10-20 meters). These wavelengths were being considered for transatlantic radio telephones. After recording signals from all directions for several months, Jansky identified three types of static: • nearby thunderstorms • distant ...
NGC 1808 - Rencontres de Moriond
... + The contribution to soft X-rays might be non-negligible, but is is any case below 30%. + The contribution to hard X-rays is negligible. + The SSC could produce only around 1/50 of the ionizing photons producing the observed emission line spectrum, and no more than 1/10 of the observed FIR luminosi ...
... + The contribution to soft X-rays might be non-negligible, but is is any case below 30%. + The contribution to hard X-rays is negligible. + The SSC could produce only around 1/50 of the ionizing photons producing the observed emission line spectrum, and no more than 1/10 of the observed FIR luminosi ...