Fundamental properties of core-collapse Supernova and GRB
... RSG phase. The models predict that core-collapse SN occur after the WR phase, and are of the type Ibc (Georgy et al. 2012, 2009). However, this scenario has yet to be observationally confirmed, specially because WR stars have not been directly detected as SN Ibc progenitors yet (Smartt 2009; Eldridg ...
... RSG phase. The models predict that core-collapse SN occur after the WR phase, and are of the type Ibc (Georgy et al. 2012, 2009). However, this scenario has yet to be observationally confirmed, specially because WR stars have not been directly detected as SN Ibc progenitors yet (Smartt 2009; Eldridg ...
edmund c. stoner and the discovery of the maximum mass of white
... principle could be applied to solve a major puzzle, the origin of the extreme high density of white dwarfs,8 which could not be explained by classical physics. Arthur Eddington expressed this puzzle as follows: “I do not see how a star which has once got into this compressed state is ever going to g ...
... principle could be applied to solve a major puzzle, the origin of the extreme high density of white dwarfs,8 which could not be explained by classical physics. Arthur Eddington expressed this puzzle as follows: “I do not see how a star which has once got into this compressed state is ever going to g ...
Local Group Encyclopedia of Astronomy & Astrophysics eaa.iop.org Mario L Mateo
... our own. These nearby systems also provide our clearest views of how galaxies interact with one another in the relatively small volume of space of the Local Group. The brightest members of the Local Group are so close to us that on a clear, dark night away from city lights it is possible to see them ...
... our own. These nearby systems also provide our clearest views of how galaxies interact with one another in the relatively small volume of space of the Local Group. The brightest members of the Local Group are so close to us that on a clear, dark night away from city lights it is possible to see them ...
Planet gaps in the dust layer of 3D protoplanetary disks
... Because of the size of particles in the weakly coupled regime for the particular case of the MMSN (1 m, see Sect. 2), that study had no direct application to observations. Images of dusty disks at infrared wavelengths do not probe such large particles, but instead trace the smaller, strongly coupled ...
... Because of the size of particles in the weakly coupled regime for the particular case of the MMSN (1 m, see Sect. 2), that study had no direct application to observations. Images of dusty disks at infrared wavelengths do not probe such large particles, but instead trace the smaller, strongly coupled ...
Slide 1
... Moving Towards Black Holes • If the remaining neutron star has a “critical mass” (about 3MSun) it can continue to collapse • Nothing left to oppose the crush of gravity! Continues to collapse until it becomes a Black ...
... Moving Towards Black Holes • If the remaining neutron star has a “critical mass” (about 3MSun) it can continue to collapse • Nothing left to oppose the crush of gravity! Continues to collapse until it becomes a Black ...
GOODS: Great Observatories Origins Deep Survey
... STScI/ESO/ST-ECF/JPL/SSC/Gemini/Boston U./U. Ariz./U. Fla./U. Hawai/UCLA/UCSC/IAP/Saclay/Yale/AUI ...
... STScI/ESO/ST-ECF/JPL/SSC/Gemini/Boston U./U. Ariz./U. Fla./U. Hawai/UCLA/UCSC/IAP/Saclay/Yale/AUI ...
The Diffuse Interstellar Bands in History and in the UV
... In 1921, while Mary Lea Heger was making observations of “stationary” (i.e. interstellar) atomic sodium absorption lines in stellar spectra, she noted the presence of two broad features at 5780 and 5797 Å that appeared to be interstellar in origin (Heger 1922). Heger took little notice of these fea ...
... In 1921, while Mary Lea Heger was making observations of “stationary” (i.e. interstellar) atomic sodium absorption lines in stellar spectra, she noted the presence of two broad features at 5780 and 5797 Å that appeared to be interstellar in origin (Heger 1922). Heger took little notice of these fea ...
Origin and Evolution of the Abundance Gradient along the Milky
... 43 nearby, late-type galaxies from GALEX and conclude that, on the average, their results are compatible with Classical KS law and can extend this simple law to much lower gas mass surface density. But for an individual galaxy, some will show a very untypical pattern in the lg(SFR)-lg(Σgas ) plot, e ...
... 43 nearby, late-type galaxies from GALEX and conclude that, on the average, their results are compatible with Classical KS law and can extend this simple law to much lower gas mass surface density. But for an individual galaxy, some will show a very untypical pattern in the lg(SFR)-lg(Σgas ) plot, e ...
Chandra HETGS Multiphase Spectroscopy Of The Young
... hemispheres meet at the magnetic equator, potentially at high velocity. This head-on collision between fast wind streams can lead to very high (T 3 107 K) shock temperatures, much higher than those seen in observations of normal O stars (e.g., Pup; Hillier et al. (1993). X-ray production in O-type ...
... hemispheres meet at the magnetic equator, potentially at high velocity. This head-on collision between fast wind streams can lead to very high (T 3 107 K) shock temperatures, much higher than those seen in observations of normal O stars (e.g., Pup; Hillier et al. (1993). X-ray production in O-type ...
THREE Li-RICH K GIANTS - Indian Institute of Astrophysics
... Stellar parameters Teff , log g, and [Fe/ H] were obtained from the spectra by a standard procedure using ATLAS model atmospheres computed using the ‘‘no convective overshoot’’ option (see Robert L. Kurucz’s Web site2). The effective temperature (Teff) was obtained from the requirement that all Fe i ...
... Stellar parameters Teff , log g, and [Fe/ H] were obtained from the spectra by a standard procedure using ATLAS model atmospheres computed using the ‘‘no convective overshoot’’ option (see Robert L. Kurucz’s Web site2). The effective temperature (Teff) was obtained from the requirement that all Fe i ...
Document
... 1938 H. A. Bethe and C. L. Critchfield: “The formation of deuterons by proton combination” ...
... 1938 H. A. Bethe and C. L. Critchfield: “The formation of deuterons by proton combination” ...
What causes the large extensions of red supergiant
... in the CO lines, but these are much weaker than the observed features. This effect is also reflected in the panels showing the uniform disk diameter. The size increases of UD fits at the CO bandheads are about 40% for V602 Car and 20% for HD 95687, while the PHOENIX models predict UD size increases b ...
... in the CO lines, but these are much weaker than the observed features. This effect is also reflected in the panels showing the uniform disk diameter. The size increases of UD fits at the CO bandheads are about 40% for V602 Car and 20% for HD 95687, while the PHOENIX models predict UD size increases b ...
d+p 3He
... 1938 H. A. Bethe and C. L. Critchfield: “The formation of deuterons by proton combination” ...
... 1938 H. A. Bethe and C. L. Critchfield: “The formation of deuterons by proton combination” ...
pp-chain
... 1938 H. A. Bethe and C. L. Critchfield: “The formation of deuterons by proton combination” ...
... 1938 H. A. Bethe and C. L. Critchfield: “The formation of deuterons by proton combination” ...
A Study of the Nature and Representative Features of Supernova
... The nature of supernovae was not initially understood. They were referred to as “guest stars” and seen as omens in a variety of cultures in Asian and European countries. Approximately 231 confirmed nearby (Galactic) supernovae remnants exist, with a few dozen other heavily suspected. For a listing a ...
... The nature of supernovae was not initially understood. They were referred to as “guest stars” and seen as omens in a variety of cultures in Asian and European countries. Approximately 231 confirmed nearby (Galactic) supernovae remnants exist, with a few dozen other heavily suspected. For a listing a ...
Star formation
Star formation is the process by which dense regions within molecular clouds in interstellar space, sometimes referred to as ""stellar nurseries"" or ""star-forming regions"", collapse to form stars. As a branch of astronomy, star formation includes the study of the interstellar medium (ISM) and giant molecular clouds (GMC) as precursors to the star formation process, and the study of protostars and young stellar objects as its immediate products. It is closely related to planet formation, another branch of astronomy. Star formation theory, as well as accounting for the formation of a single star, must also account for the statistics of binary stars and the initial mass function.In June 2015, astronomers reported evidence for Population III stars in the Cosmos Redshift 7 galaxy at z = 6.60. Such stars are likely to have existed in the very early universe (i.e., at high redshift), and may have started the production of chemical elements heavier than hydrogen that are needed for the later formation of planets and life as we know it.