SAGE_prop
... unanswerable questions at the moment. From a comparison of the Sun with other stars, we know that it is quite inactive. Its typical coronal temperature is ~ 1 MK, reaching ~ 5 MK in active regions and ~ 15 MK in flares. Most late-type stars with outer convection zones, i.e., stars of spectral type F ...
... unanswerable questions at the moment. From a comparison of the Sun with other stars, we know that it is quite inactive. Its typical coronal temperature is ~ 1 MK, reaching ~ 5 MK in active regions and ~ 15 MK in flares. Most late-type stars with outer convection zones, i.e., stars of spectral type F ...
High Energy Astrophysics T. J.
... XMM-Newton, Chandra and INTEGRAL. The first two are large X-ray instruments, one specialised in imaging (Chandra) the other in spectroscopy (XMM), because of its very large collecting area. INTEGRAL is sensitive above few keV and up to some MeV. However, other observation tools in all domains of the ...
... XMM-Newton, Chandra and INTEGRAL. The first two are large X-ray instruments, one specialised in imaging (Chandra) the other in spectroscopy (XMM), because of its very large collecting area. INTEGRAL is sensitive above few keV and up to some MeV. However, other observation tools in all domains of the ...
LISENFELD Ute: Suppression of star formation in compact groups
... interes/ng systems to study galaxy transforma/on because interac/ons between galaxies and with the intragroup medium are frequent. • A gap/canyon was found in their Spitzer IR colors between ac/ve and quiescent galaxies, indica/ng a fast transi/on between both phases (Johnson+07, Walker+1 ...
... interes/ng systems to study galaxy transforma/on because interac/ons between galaxies and with the intragroup medium are frequent. • A gap/canyon was found in their Spitzer IR colors between ac/ve and quiescent galaxies, indica/ng a fast transi/on between both phases (Johnson+07, Walker+1 ...
PDF only - at www.arxiv.org.
... is foreseen in the near future. Some of them, like SIMBOL-X1, Constellation-X/HXT2, NeXT3, XEUS/HXT4, will extend the current techniques for X-ray focusing (to date, adopted only below 10 keV) to the hard (E > 10 keV) X-ray band by adopting very shallow incidence angles (0.1 ÷ 0.4 deg) and graded mu ...
... is foreseen in the near future. Some of them, like SIMBOL-X1, Constellation-X/HXT2, NeXT3, XEUS/HXT4, will extend the current techniques for X-ray focusing (to date, adopted only below 10 keV) to the hard (E > 10 keV) X-ray band by adopting very shallow incidence angles (0.1 ÷ 0.4 deg) and graded mu ...
LOCALIZATION AND OBSERVATIONS OF GRB010921 BY THE …
... Early afterglows will be carefully studied the missing link between the prompt emission and the afterglow will be identified; The jet configuration will be identified universal structured jet model could be validated by future data; With accumulation of a large sample of spectral informati ...
... Early afterglows will be carefully studied the missing link between the prompt emission and the afterglow will be identified; The jet configuration will be identified universal structured jet model could be validated by future data; With accumulation of a large sample of spectral informati ...
White Dwarf Stars
... ix billion years from now, someone looking up at the sky on a summer’s day would not see the same bright Sun we now see. In its place would be a tiny orb—a “white dwarf”—shining feebly in a black sky. Whether anyone will be around to see such an alien sky is another question: All life on Earth would ...
... ix billion years from now, someone looking up at the sky on a summer’s day would not see the same bright Sun we now see. In its place would be a tiny orb—a “white dwarf”—shining feebly in a black sky. Whether anyone will be around to see such an alien sky is another question: All life on Earth would ...
Gamma-ray burst has highest redshift yet seen
... wait patiently for observers. They shine for millions of years. But a GRB’s afterglow grows fainter with every passing hour. “So we’re obliged to move fast,” says Fox. How is one to promptly identify high-z GRBs and catch their IR afterglow fast enough to yield spectra adequate for studying cosmic r ...
... wait patiently for observers. They shine for millions of years. But a GRB’s afterglow grows fainter with every passing hour. “So we’re obliged to move fast,” says Fox. How is one to promptly identify high-z GRBs and catch their IR afterglow fast enough to yield spectra adequate for studying cosmic r ...
Galaxies
... The final galaxy class identified by Hubble—irregular galaxies—named in this way because their visual appearance does not allow us to place them into any of the other categories just discussed. Irregulars tend to be rich in interstellar matter and young, blue stars, but they lack any regular structu ...
... The final galaxy class identified by Hubble—irregular galaxies—named in this way because their visual appearance does not allow us to place them into any of the other categories just discussed. Irregulars tend to be rich in interstellar matter and young, blue stars, but they lack any regular structu ...
Neutron Stars – Thermal Emitters
... component related to the NS cooling is apparent in a few sources, an additional component with a higher temperature and a smaller emitting area can also be observed (De Luca et al. 2005), probably related to re-heating of the magnetic polar caps by bombardment of magnetospheric particles. We note th ...
... component related to the NS cooling is apparent in a few sources, an additional component with a higher temperature and a smaller emitting area can also be observed (De Luca et al. 2005), probably related to re-heating of the magnetic polar caps by bombardment of magnetospheric particles. We note th ...
Lokal fulltext - Chalmers Publication Library
... up in the HR diagram towards larger luminosities. This will happen sooner the more massive the star is: the Sun has a main sequence lifetime of about 10 billion years, compared with only ∼30 million years for a 10 M star. There are several tracks a star may follow in the HR diagram, depending on it ...
... up in the HR diagram towards larger luminosities. This will happen sooner the more massive the star is: the Sun has a main sequence lifetime of about 10 billion years, compared with only ∼30 million years for a 10 M star. There are several tracks a star may follow in the HR diagram, depending on it ...
imaging spectroscopy of the centers of nearby agn
... It therefore seems likely that nuclear starbursts are episodic in nature. Given that the star formation occurs on scales of < 50 pc, it is inevitable that it and the AGN will have some mutual influence on each other. Our data hint at a possible relationship between the characteristic age of the star ...
... It therefore seems likely that nuclear starbursts are episodic in nature. Given that the star formation occurs on scales of < 50 pc, it is inevitable that it and the AGN will have some mutual influence on each other. Our data hint at a possible relationship between the characteristic age of the star ...
Cygnus X-1 poster (Massive Star Workshop)
... for Interdisciplinary Exploration and Research in Astrophysics (CIERA) & Department of Physics and Astronomy, Northwestern University 2 Harvard-Smithsonian Center for Astrophysics ...
... for Interdisciplinary Exploration and Research in Astrophysics (CIERA) & Department of Physics and Astronomy, Northwestern University 2 Harvard-Smithsonian Center for Astrophysics ...
space telescope imaging spectrograph survey of far
... LX =Lbol 105 , below which detections of the coronal forbidden line are rare. There is no evidence of large, systematic Doppler shifts in either Fe xii 1242 or Fe xxi 1354. This suggests that the emissions arise dominantly in confined structures, analogous to magnetic loops on the Sun, rather th ...
... LX =Lbol 105 , below which detections of the coronal forbidden line are rare. There is no evidence of large, systematic Doppler shifts in either Fe xii 1242 or Fe xxi 1354. This suggests that the emissions arise dominantly in confined structures, analogous to magnetic loops on the Sun, rather th ...
Explosive sources of the highest energy radiation
... front formed from the interacaverage once a year. Remarktion of the pulsar wind with the stellar wind of the Be companion. ably, there is no sign of simultaneous While the detection of gamma-ray emission variability at any other wavelengths despite by Fermi was anticipated, the highly variable numer ...
... front formed from the interacaverage once a year. Remarktion of the pulsar wind with the stellar wind of the Be companion. ably, there is no sign of simultaneous While the detection of gamma-ray emission variability at any other wavelengths despite by Fermi was anticipated, the highly variable numer ...
A third red supergiant rich cluster in the Scutum
... we suspect that the true stellar yield will be significantly higher). We highlight the apparent absence of X-ray binaries within the star formation complex and finally, given the physical association of at least two pulsars with this region, discuss the implications of this finding for stellar evolu ...
... we suspect that the true stellar yield will be significantly higher). We highlight the apparent absence of X-ray binaries within the star formation complex and finally, given the physical association of at least two pulsars with this region, discuss the implications of this finding for stellar evolu ...
Gamma-Ray Bursts
... If an optical afterglow of a GRB has an apparent visual magnitude of 19, how many times fainter is it than the faintest object visible to the bare eye? ...
... If an optical afterglow of a GRB has an apparent visual magnitude of 19, how many times fainter is it than the faintest object visible to the bare eye? ...
The Components of a Spiral Galaxy
... (star formingspiral population) " • bulges are dominated by stellar absorption lines and have little 'blue' light" ...
... (star formingspiral population) " • bulges are dominated by stellar absorption lines and have little 'blue' light" ...
![Chapter 4 [PDF only] - Princeton University Press](http://s1.studyres.com/store/data/016931743_1-7c8ec22374457bf50a0a03f55488ddc7-300x300.png)
Chapter 4 [PDF only] - Princeton University Press
... The equations of pressure, opacity, and nuclear power density all depend sensitively on the abundances. Indeed, at some point, the hydrogen fuel in the core will be largely used up, and the star will lose the energy source that produces pressure, the gradient of which supports the star against gravi ...
... The equations of pressure, opacity, and nuclear power density all depend sensitively on the abundances. Indeed, at some point, the hydrogen fuel in the core will be largely used up, and the star will lose the energy source that produces pressure, the gradient of which supports the star against gravi ...
An evolutionary channel towards the accreting millisecond pulsar
... the accretion disc should experience a thermal and viscous instability. During this stage, the accreting neutron star would be observed as a transient X-ray source, which appears as short-lived outbursts separated by long-term quiescence. The neutron star was assumed to accrete at a rate of ṀNS = m ...
... the accretion disc should experience a thermal and viscous instability. During this stage, the accreting neutron star would be observed as a transient X-ray source, which appears as short-lived outbursts separated by long-term quiescence. The neutron star was assumed to accrete at a rate of ṀNS = m ...
Present Carbon and Oxygen data with efficiency numbers
... astronomical x-ray sources. For x-ray energies above 10keV there is a hard x-ray telescope (HXT) and from 0.1 to 10keV, there is a large foil optic telescope known as the SXT. The SXT has its light divided between two instruments – a calorimeter and a reflection grating spectrometer (RGS). The calor ...
... astronomical x-ray sources. For x-ray energies above 10keV there is a hard x-ray telescope (HXT) and from 0.1 to 10keV, there is a large foil optic telescope known as the SXT. The SXT has its light divided between two instruments – a calorimeter and a reflection grating spectrometer (RGS). The calor ...
Radio observations of the planetary nebula around the OH/IR Star
... We present radio observations of the unique, recently formed, planetary nebula (PN) associated with a very long-period OH/IR variable star V1018 Sco that is unequivocally still in its asymptotic giant branch phase. Two regions within the optical nebula are clearly detected in nonthermal radio contin ...
... We present radio observations of the unique, recently formed, planetary nebula (PN) associated with a very long-period OH/IR variable star V1018 Sco that is unequivocally still in its asymptotic giant branch phase. Two regions within the optical nebula are clearly detected in nonthermal radio contin ...
Chapter 15
... • These population III stars may not be observable for three reasons – Only short-lived massive population III stars can form – consequently none are left today – Population III stars exist, but are masquerading as Pop II since their atmospheres have been contaminated by gas ejected when a more mass ...
... • These population III stars may not be observable for three reasons – Only short-lived massive population III stars can form – consequently none are left today – Population III stars exist, but are masquerading as Pop II since their atmospheres have been contaminated by gas ejected when a more mass ...
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.