Barger - Chandra X-Ray Observatory (CXC)
... Thus, the current radio source population cannot account for the background light that has been suggested may be missing at 4-8 keV ...
... Thus, the current radio source population cannot account for the background light that has been suggested may be missing at 4-8 keV ...
Clase-06_Star_Formation - Departamento de Astronomía
... for early A stars, p.e.) can be traced by their brightness in UV Mechanism: they produce a UV continuum in SF galaxies at wavelengths longer than the Lyman limit (λ = 912Å) this continuum is remarkbly flat, as can be modelled by spectral synthesis codes (first noted by Lilly & Cowie [1987, Infra ...
... for early A stars, p.e.) can be traced by their brightness in UV Mechanism: they produce a UV continuum in SF galaxies at wavelengths longer than the Lyman limit (λ = 912Å) this continuum is remarkbly flat, as can be modelled by spectral synthesis codes (first noted by Lilly & Cowie [1987, Infra ...
404.06 Stephen Drake
... etc., => given present sensitivity levels ~10-9 erg cm-2 s-1, only the largest flares will be found: e.g., Swift detections of stellar flares from the active binary systems Algol, II Peg & HR 1099 and the M4.5V star EV Lac and MAXI detections of ~12 flares You can ask for long pointed observations ...
... etc., => given present sensitivity levels ~10-9 erg cm-2 s-1, only the largest flares will be found: e.g., Swift detections of stellar flares from the active binary systems Algol, II Peg & HR 1099 and the M4.5V star EV Lac and MAXI detections of ~12 flares You can ask for long pointed observations ...
Star Clusters and their stars
... appear as MS stars that look brighter and bluer than the vast majority of stars in the cluster. It looks as if they might be the result of stellar mergers – once two stars merge, they will be more massive, and therefore hotter and fusing hydrogen at a ...
... appear as MS stars that look brighter and bluer than the vast majority of stars in the cluster. It looks as if they might be the result of stellar mergers – once two stars merge, they will be more massive, and therefore hotter and fusing hydrogen at a ...
Star_Clusters
... appear as MS stars that look brighter and bluer than the vast majority of stars in the cluster. It looks as if they might be the result of stellar mergers – once two stars merge, they will be more massive, and therefore hotter and fusing hydrogen at a ...
... appear as MS stars that look brighter and bluer than the vast majority of stars in the cluster. It looks as if they might be the result of stellar mergers – once two stars merge, they will be more massive, and therefore hotter and fusing hydrogen at a ...
Document
... Flare <15s to 1 hr, repeats hrs - days Amplitude up to 4 mag Opt is thermal brem at T ~ 107K, radio is non-thermal Between flares, spectrum is K-M with CaII, H emission ...
... Flare <15s to 1 hr, repeats hrs - days Amplitude up to 4 mag Opt is thermal brem at T ~ 107K, radio is non-thermal Between flares, spectrum is K-M with CaII, H emission ...
The Sun The Sun is a very typical main sequence star. It contains 100
... The solar photosphere is the thin layer of gas near the surface from which essen9ally all the visible light that we see is emi_ed. We can observe into the photosphere a distance of about 4 ...
... The solar photosphere is the thin layer of gas near the surface from which essen9ally all the visible light that we see is emi_ed. We can observe into the photosphere a distance of about 4 ...
Carl Sagan`s Contact
... Theory of Wormholes Matter is neither created nor destroyed Objects sucked into a rotating, electrically charged blackhole do not disappear One theory is that they reappear elsewhere out of an exit point or whitehole The tunnel that links a blackhole and whitehole is known as a wormhole ...
... Theory of Wormholes Matter is neither created nor destroyed Objects sucked into a rotating, electrically charged blackhole do not disappear One theory is that they reappear elsewhere out of an exit point or whitehole The tunnel that links a blackhole and whitehole is known as a wormhole ...
Astronomy - Scioly.org
... e. They are fully connective, and never develop a hydrogen shell fusion zone. 53. What type of spectrum does the gas in a planetary nebula produce? a. A continuous spectrum. b. An emission line spectrum. c. An absorption line spectrum. d. An emission line spectrum superimposed on a continuous spectr ...
... e. They are fully connective, and never develop a hydrogen shell fusion zone. 53. What type of spectrum does the gas in a planetary nebula produce? a. A continuous spectrum. b. An emission line spectrum. c. An absorption line spectrum. d. An emission line spectrum superimposed on a continuous spectr ...
Chapter 10: The Sun-
... circular orbit (ISCO) for a nonrotating hole is fGW(ISCO)=4.4x103 Hz (Msun/M) For rotating, up to fGW(ISCO)~2x104 Hz (Msun/M) More generally, object of average density has maximum frequency ~(G)1/2 Neutron star: ~2000 Hz White dwarf: up to ~1 Hz ...
... circular orbit (ISCO) for a nonrotating hole is fGW(ISCO)=4.4x103 Hz (Msun/M) For rotating, up to fGW(ISCO)~2x104 Hz (Msun/M) More generally, object of average density has maximum frequency ~(G)1/2 Neutron star: ~2000 Hz White dwarf: up to ~1 Hz ...
Ch 13 Death of Stars(4-5?-13)
... the star electrons can combine with protons, making neutrons and neutrinos forming a neutron star ...
... the star electrons can combine with protons, making neutrons and neutrinos forming a neutron star ...
Ch. 13 Death of Stars(11-16-10)-3
... the star electrons can combine with protons, making neutrons and neutrinos forming a neutron star ...
... the star electrons can combine with protons, making neutrons and neutrinos forming a neutron star ...
IND 6 - 1 Stars and Stellar Evolution In order to better understand
... A low mass star (less than 8 times the mass of our Sun ( < 8 Msun)) eventually ejects its outer layers to produce a planetary nebula. The now naked stellar core remaining is called a white dwarf (because it is very hot but dim). In contrast, a high-mass star, more than 8 times the mass of our Su ...
... A low mass star (less than 8 times the mass of our Sun ( < 8 Msun)) eventually ejects its outer layers to produce a planetary nebula. The now naked stellar core remaining is called a white dwarf (because it is very hot but dim). In contrast, a high-mass star, more than 8 times the mass of our Su ...
the chromospheres of classical cepheids. 111. a search for transition
... argued that the regions in which they originate have a minimum extent which ranges from several tenths of a stellar radius to several stellar radii in various stars. This is much larger than the solar chromosphere, but not as extended as the chromospheres of late-type giants. In Paper I we presented ...
... argued that the regions in which they originate have a minimum extent which ranges from several tenths of a stellar radius to several stellar radii in various stars. This is much larger than the solar chromosphere, but not as extended as the chromospheres of late-type giants. In Paper I we presented ...
Non-thermal hard X-ray emission from stellar coronae
... Ionization of protoplanetary disks and ISM ...
... Ionization of protoplanetary disks and ISM ...
Document
... between yearly epochs at the 5 level with the CFHT Legacy Survey optical catalog. • Rule out sources with optical hosts with the colors and morphology of a star or quasar. • Follow up galaxy hosts that do not have an hard X-ray detection with optical spectroscopy to look for signs of an AGN. • Trig ...
... between yearly epochs at the 5 level with the CFHT Legacy Survey optical catalog. • Rule out sources with optical hosts with the colors and morphology of a star or quasar. • Follow up galaxy hosts that do not have an hard X-ray detection with optical spectroscopy to look for signs of an AGN. • Trig ...
1 - ESO
... In the past year, three more stars with warm dust in the terrestrial region have been identified With Spitzer, Beichman et al 2005 found an ~2 Gyr old K-type star (HD 69830) with tau ~10-4 and silicate emission features seen in the wavelength range accessible to IRS. (Note: excess emission at 25 mi ...
... In the past year, three more stars with warm dust in the terrestrial region have been identified With Spitzer, Beichman et al 2005 found an ~2 Gyr old K-type star (HD 69830) with tau ~10-4 and silicate emission features seen in the wavelength range accessible to IRS. (Note: excess emission at 25 mi ...
5. Star Formation and the Interstellar Medium in the Milky Way
... line and thermal dust continuum emission and are often associated with compact or evolved HII regions. However, there are few nearby examples that would provide insights into their origins within giant molecular clouds and the complex interactions that must occur between embedded protostellar object ...
... line and thermal dust continuum emission and are often associated with compact or evolved HII regions. However, there are few nearby examples that would provide insights into their origins within giant molecular clouds and the complex interactions that must occur between embedded protostellar object ...
Chandra - Astronomy at Swarthmore College
... (Florida Institute of Technology), Marc Gagné (West Chester), Asif ud-Doula (Penn St. Worthington-Scranton) with Emma Wollman (Caltech, Swarthmore ’09), James MacArthur (Stanford, Swarthmore ’11), Zack Li (Swarthmore ’16) ...
... (Florida Institute of Technology), Marc Gagné (West Chester), Asif ud-Doula (Penn St. Worthington-Scranton) with Emma Wollman (Caltech, Swarthmore ’09), James MacArthur (Stanford, Swarthmore ’11), Zack Li (Swarthmore ’16) ...
the effect of an soft X-ray source near the compact object in LS 5039
... In Y&T 2010, e± scattered off stellar photons → each flux modulates by the anisotropy of IC scattering In this study, they scatter off isotropic photons → emerging photons with GeV & keV have isotropic distribution → No modulation in GeV & X-ray band ...
... In Y&T 2010, e± scattered off stellar photons → each flux modulates by the anisotropy of IC scattering In this study, they scatter off isotropic photons → emerging photons with GeV & keV have isotropic distribution → No modulation in GeV & X-ray band ...
Station A Star Charts I
... D. This color is only produced by degenerate matter, not plasma. C13. Which color do the hottest stars appear to be? A. Bluish white ...
... D. This color is only produced by degenerate matter, not plasma. C13. Which color do the hottest stars appear to be? A. Bluish white ...
Poster
... The jet has a non-axisymmetric (m=2 like) structure in the both perturbation cases. This structure is not caused by K-H instability. The corresponding m=2 like structure in the disk appears before that in the jet appears. This is confirmed by calculating the Fourier spectra of the magnetic energy. T ...
... The jet has a non-axisymmetric (m=2 like) structure in the both perturbation cases. This structure is not caused by K-H instability. The corresponding m=2 like structure in the disk appears before that in the jet appears. This is confirmed by calculating the Fourier spectra of the magnetic energy. T ...
ASTRONOMY 120
... A nova is a binary star system that suddenly brightens and then slowly fades back to normal. It is caused by an evolving star in a binary that is expanding past its Roche lobe and losing gas to a companion white dwarf. After a while, the material (primarily hydrogen) builds up on the white dwarf and ...
... A nova is a binary star system that suddenly brightens and then slowly fades back to normal. It is caused by an evolving star in a binary that is expanding past its Roche lobe and losing gas to a companion white dwarf. After a while, the material (primarily hydrogen) builds up on the white dwarf and ...
Cygnus X-1
Cygnus X-1 (abbreviated Cyg X-1) is a well-known galactic X-ray source, thought to be a black hole, in the constellation Cygnus. It was discovered in 1964 during a rocket flight and is one of the strongest X-ray sources seen from Earth, producing a peak X-ray flux density of 6977229999999999999♠2.3×10−23 Wm−2 Hz−1 (7003230000000000000♠2.3×103 Jansky). Cygnus X-1 was the first X-ray source widely accepted to be a black hole and it remains among the most studied astronomical objects in its class. The compact object is now estimated to have a mass about 14.8 times the mass of the Sun and has been shown to be too small to be any known kind of normal star, or other likely object besides a black hole. If so, the radius of its event horizon is about 7004440000000000000♠44 km.Cygnus X-1 belongs to a high-mass X-ray binary system about 7019574266339685654♠6070 ly from the Sun that includes a blue supergiant variable star designated HDE 226868 which it orbits at about 0.2 AU, or 20% of the distance from the Earth to the Sun. A stellar wind from the star provides material for an accretion disk around the X-ray source. Matter in the inner disk is heated to millions of degrees, generating the observed X-rays. A pair of jets, arranged perpendicular to the disk, are carrying part of the energy of the infalling material away into interstellar space.This system may belong to a stellar association called Cygnus OB3, which would mean that Cygnus X-1 is about five million years old and formed from a progenitor star that had more than 7001400000000000000♠40 solar masses. The majority of the star's mass was shed, most likely as a stellar wind. If this star had then exploded as a supernova, the resulting force would most likely have ejected the remnant from the system. Hence the star may have instead collapsed directly into a black hole.Cygnus X-1 was the subject of a friendly scientific wager between physicists Stephen Hawking and Kip Thorne in 1975, with Hawking betting that it was not a black hole. He conceded the bet in 1990 after observational data had strengthened the case that there was indeed a black hole in the system. This hypothesis has not been confirmed due to a lack of direct observation but has generally been accepted from indirect evidence.