Chap 16: Galaxies
... • Do other galaxies contain supermassive black holes and dark matter, as does our own galaxy? • Why are there different kinds of galaxies? ...
... • Do other galaxies contain supermassive black holes and dark matter, as does our own galaxy? • Why are there different kinds of galaxies? ...
APS Neutrino Study
... sections in the energy range of a few tens of MeV. These cross sections, which are uncertain at the level of several times 10% from theory, are very important for understanding supernovae, specifically the neutrino opacities, nucleosynthesis, and detection. For example, in the event of a Milky Way s ...
... sections in the energy range of a few tens of MeV. These cross sections, which are uncertain at the level of several times 10% from theory, are very important for understanding supernovae, specifically the neutrino opacities, nucleosynthesis, and detection. For example, in the event of a Milky Way s ...
discovery of four new massive and dense cold cores
... limeter wavelengths by Sandell (2000). Hereafter, we only concentrate on the four newly discovered massive cold cores. Figures 1–4 (top panel ) present maps of the 1.2 mm emission from regions of 100 –150 in size centered on the IRAS sources. Also shown in these figures are gray scale images of mid ...
... limeter wavelengths by Sandell (2000). Hereafter, we only concentrate on the four newly discovered massive cold cores. Figures 1–4 (top panel ) present maps of the 1.2 mm emission from regions of 100 –150 in size centered on the IRAS sources. Also shown in these figures are gray scale images of mid ...
Chapter 9 Early stages of evolution and the main sequence phase
... Therefore the shape of the Hayashi line in the HRD is determined by how the opacity in the photosphere depends on ρ and T . Since fully convective stars have very cool photospheres, the opacity is mainly given by H− absorption (Sect. 5.3) which increases strongly with temperature. According to eq. ( ...
... Therefore the shape of the Hayashi line in the HRD is determined by how the opacity in the photosphere depends on ρ and T . Since fully convective stars have very cool photospheres, the opacity is mainly given by H− absorption (Sect. 5.3) which increases strongly with temperature. According to eq. ( ...
Gravitational Waves from 3D MHD Core
... universe, liberating the prodigious amount of ∼ 1053 erg, the binding energy of their compact remnants, neutron stars or stellar mass black holes. While 99% of this energy is emitted in neutrinos, 1% goes into the internal and asymptotic kinetic energy of the ejecta, and it is reasonable to assume t ...
... universe, liberating the prodigious amount of ∼ 1053 erg, the binding energy of their compact remnants, neutron stars or stellar mass black holes. While 99% of this energy is emitted in neutrinos, 1% goes into the internal and asymptotic kinetic energy of the ejecta, and it is reasonable to assume t ...
The Role of Radioactive Isotopes in Astrophysics
... environmental situations in stars within which selected isotopes would be abundant, fleshing out ideas that Suess had envisioned earlier for two neutron-capture processes. Suess had, however, been unable to formulate these clearly enough to win contemporary acclaim. The slow neutron-capture process, ...
... environmental situations in stars within which selected isotopes would be abundant, fleshing out ideas that Suess had envisioned earlier for two neutron-capture processes. Suess had, however, been unable to formulate these clearly enough to win contemporary acclaim. The slow neutron-capture process, ...
White dwarf dynamical interactions and fast optical transients
... properties of the dynamical interaction are similar for similar masses of the interacting white dwarfs. More importantly, in both cases variable amounts of nickel are synthesized in the ensuing thermonuclear flash, thus powering quite different light curves. This could help to explain the observed f ...
... properties of the dynamical interaction are similar for similar masses of the interacting white dwarfs. More importantly, in both cases variable amounts of nickel are synthesized in the ensuing thermonuclear flash, thus powering quite different light curves. This could help to explain the observed f ...
An Atlas of Stellar Spectra
... of a group of stars of the same spectral type and luminosity class can be determined with great precision, even when the group consists of a relatively small number of stars. Even for individual stars distances of good accuracy can be derived. A corresponding gain is made in problems concerned with ...
... of a group of stars of the same spectral type and luminosity class can be determined with great precision, even when the group consists of a relatively small number of stars. Even for individual stars distances of good accuracy can be derived. A corresponding gain is made in problems concerned with ...
Annual Report 2012 - Max Planck Institute for Astrophysics
... instrumental activities carried out in other MaxPlanck institutes. From its inception the MPA has The Max-Planck-Institut für Astrophysik, called had an internationally-recognized numerical astrothe MPA for short, was founded in 1958 under the physics program that is unparalleled by any other direct ...
... instrumental activities carried out in other MaxPlanck institutes. From its inception the MPA has The Max-Planck-Institut für Astrophysik, called had an internationally-recognized numerical astrothe MPA for short, was founded in 1958 under the physics program that is unparalleled by any other direct ...
Evolution of stars
... medium are cold and of a very low density because a. the lines are blue shifted. b. the lines are red shifted. c. the lines are extremely broad. d. the lines are extremely narrow. e. the lines are much darker than the stellar lines. Stars are born in a. reflection nebulae. b. dense molecular clouds. ...
... medium are cold and of a very low density because a. the lines are blue shifted. b. the lines are red shifted. c. the lines are extremely broad. d. the lines are extremely narrow. e. the lines are much darker than the stellar lines. Stars are born in a. reflection nebulae. b. dense molecular clouds. ...
POSTERS SESSION I: Atmospheres of Massive Stars
... wind, probably triggered by a companion star’s periastron approach. This indicates a surface instability that was not predicted and is stronger than one would normally have expected based on tidal and radiative effects. The hypothetical companion object continuously alters the primary star’s surface ...
... wind, probably triggered by a companion star’s periastron approach. This indicates a surface instability that was not predicted and is stronger than one would normally have expected based on tidal and radiative effects. The hypothetical companion object continuously alters the primary star’s surface ...
GammaRay Bursts, the Strongest Explosions in the Universe.
... Paczynski, Ramesh Narayan (from Harvard) I18 suggested internal shocks within the outflow as an alternative way to convert the kinetic energy to radiation. The basic idea was the collisionless shocks accelerate electrons and produce magnetic fields. The electrons movi ...
... Paczynski, Ramesh Narayan (from Harvard) I18 suggested internal shocks within the outflow as an alternative way to convert the kinetic energy to radiation. The basic idea was the collisionless shocks accelerate electrons and produce magnetic fields. The electrons movi ...
20_Testbank
... the Milky Way. Therefore, they serve as a bridge between us and standard candles in other galaxies. Once we determine the distance to another galaxy for which we have observed a whitedwarf supernova, we then can calibrate the average luminosity of white-dwarf supernovae. White-dwarf supernovae and C ...
... the Milky Way. Therefore, they serve as a bridge between us and standard candles in other galaxies. Once we determine the distance to another galaxy for which we have observed a whitedwarf supernova, we then can calibrate the average luminosity of white-dwarf supernovae. White-dwarf supernovae and C ...
The evolution and explosion of massive stars
... Like all true stars, massive stars are gravitationally confined thermonuclear reactors whose composition evolves as energy is lost to radiation and neutrinos. Unlike lower-mass stars ( M ⱗ8M 䉺 ) , however, no point is ever reached at which a massive star can be fully supported by electron degeneracy ...
... Like all true stars, massive stars are gravitationally confined thermonuclear reactors whose composition evolves as energy is lost to radiation and neutrinos. Unlike lower-mass stars ( M ⱗ8M 䉺 ) , however, no point is ever reached at which a massive star can be fully supported by electron degeneracy ...
SN 2006gy: DISCOVERY OF THE MOST LUMINOUS
... We report the discovery and early observations of the peculiar Type IIn supernova (SN) 2006gy in NGC 1260. With a peak visual magnitude of about 22, it is the most luminous supernova ever recorded. Its very slow rise to maximum took 70 days, and it stayed brighter than 21 mag for about 100 days. ...
... We report the discovery and early observations of the peculiar Type IIn supernova (SN) 2006gy in NGC 1260. With a peak visual magnitude of about 22, it is the most luminous supernova ever recorded. Its very slow rise to maximum took 70 days, and it stayed brighter than 21 mag for about 100 days. ...
White dwarf binary
... 2 types of SN Nova or supernova? Standard candles Neutron stars Discovery Crab pulsar Pulsars Pulsars are NS! Magnetic fields Thought question Binaries Spin up Thought question ...
... 2 types of SN Nova or supernova? Standard candles Neutron stars Discovery Crab pulsar Pulsars Pulsars are NS! Magnetic fields Thought question Binaries Spin up Thought question ...
SN 2011dh and the progenitors of Type IIb supernovae Mattias Ergon
... creates a powerful shock that disrupts the star and ejects the heated material into the surrounding circumstellar medium. The observed properties depend on the mass lost by the star, e.g. through stellar winds or mass transfer in binary systems, and the subject of this thesis is the class of Type II ...
... creates a powerful shock that disrupts the star and ejects the heated material into the surrounding circumstellar medium. The observed properties depend on the mass lost by the star, e.g. through stellar winds or mass transfer in binary systems, and the subject of this thesis is the class of Type II ...
SNEWS - University of Minnesota
... – Ia are Standard Bombs used in cosmological work – These days the “year + letter” naming scheme is getting cumbersome, almost need to bar code the things ...
... – Ia are Standard Bombs used in cosmological work – These days the “year + letter” naming scheme is getting cumbersome, almost need to bar code the things ...
Galaxies
... galaxies in a given cluster averages a few hundred thousand parsecs, which is only about 10 times greater than the size of a typical galaxy. Galaxies simply do not have that much room to roam around without bumping into one another. By contrast, stars within a galaxy are spread out much more thinl ...
... galaxies in a given cluster averages a few hundred thousand parsecs, which is only about 10 times greater than the size of a typical galaxy. Galaxies simply do not have that much room to roam around without bumping into one another. By contrast, stars within a galaxy are spread out much more thinl ...
Gamma-Ray Bursts and Puzzles of Core
... evolution of the blueshifted Hα line were already found (using SYNOW code) in the analysis of a time series of optical spectra for usual CC-SNe with type Ic and Ib (Branch et al., 2001, 2002, Elmhamdi et al., 2006, …). ...
... evolution of the blueshifted Hα line were already found (using SYNOW code) in the analysis of a time series of optical spectra for usual CC-SNe with type Ic and Ib (Branch et al., 2001, 2002, Elmhamdi et al., 2006, …). ...
Insights into thermonuclear supernovae from the incomplete Si
... of a few well-studied SNIa (Stehle et al. 2005a; Altavilla et al. 2007; Mazzali et al. 2008; Tanaka et al. 2011). It is to be expected that the set of SNIa for which a detailed chemical composition of the ejecta is available will increase steadily in the next several years. An alternative way to gai ...
... of a few well-studied SNIa (Stehle et al. 2005a; Altavilla et al. 2007; Mazzali et al. 2008; Tanaka et al. 2011). It is to be expected that the set of SNIa for which a detailed chemical composition of the ejecta is available will increase steadily in the next several years. An alternative way to gai ...
Binary star progenitors of long GRBs
... Fast rotating massive stars can evolve chemically homogeneous and become long GRBs Two classes of progenitors: single and binary stars In massive binaries it’s possible to spin up a star and obtain a collapsar This scenario is likely to produce a runaway WR which travel several hundred pc be ...
... Fast rotating massive stars can evolve chemically homogeneous and become long GRBs Two classes of progenitors: single and binary stars In massive binaries it’s possible to spin up a star and obtain a collapsar This scenario is likely to produce a runaway WR which travel several hundred pc be ...
The X-ray/radio and UV luminosity expected from symbiotic systems
... likely to be the signatures of gas outflows from the SD systems, although it is possible for some DD systems to show signs of CSM as well, e.g., Shen et al. (2013). Furthermore, Foley et al. (2012a) even find that SNe Ia with blueshifted circumstellar/interstellar absorption systematically have high ...
... likely to be the signatures of gas outflows from the SD systems, although it is possible for some DD systems to show signs of CSM as well, e.g., Shen et al. (2013). Furthermore, Foley et al. (2012a) even find that SNe Ia with blueshifted circumstellar/interstellar absorption systematically have high ...
variable star type designations in vsx
... A pipe character ( | ) between two different types signifies a logical OR; the classification is uncertain and all possible types are indicated. An example of this is ELL|DSCT, where the star may be an ellipsoidal binary system or a DSCT-type pulsating variable with half the given period. A plus cha ...
... A pipe character ( | ) between two different types signifies a logical OR; the classification is uncertain and all possible types are indicated. An example of this is ELL|DSCT, where the star may be an ellipsoidal binary system or a DSCT-type pulsating variable with half the given period. A plus cha ...
The presence of gamma rays in space was known before they were
... Gamma rays were first discovered in 1900 by Villiard, although they become known as gamma rays due to Rutherford. It was not until 1948 when Freeberg and Primakoff theorised that gamma rays are produced in space. The first actual gamma rays detected from space were detected by sensors mounted on a h ...
... Gamma rays were first discovered in 1900 by Villiard, although they become known as gamma rays due to Rutherford. It was not until 1948 when Freeberg and Primakoff theorised that gamma rays are produced in space. The first actual gamma rays detected from space were detected by sensors mounted on a h ...
Supernova
A supernova is a stellar explosion that briefly outshines an entire galaxy, radiating as much energy as the Sun or any ordinary star is expected to emit over its entire life span, before fading from view over several weeks or months. The extremely luminous burst of radiation expels much or all of a star's material at a velocity of up to 7007300000000000000♠30,000 km/s (10% of the speed of light), driving a shock wave into the surrounding interstellar medium. This shock wave sweeps up an expanding shell of gas and dust called a supernova remnant. Supernovae are potentially strong galactic sources of gravitational waves. A great proportion of primary cosmic rays comes from supernovae.Supernovae are more energetic than novae. Nova means ""new"" in Latin, referring to what appears to be a very bright new star shining in the celestial sphere; the prefix ""super-"" distinguishes supernovae from ordinary novae, which are far less luminous. The word supernova was coined by Walter Baade and Fritz Zwicky in 1931. It is pronounced /ˌsuːpərnoʊvə/ with the plural supernovae /ˌsuːpərnoʊviː/ or supernovas (abbreviated SN, plural SNe after ""supernovae"").Supernovae can be triggered in one of two ways: by the sudden re-ignition of nuclear fusion in a degenerate star; or by the gravitational collapse of the core of a massive star. In the first case, a degenerate white dwarf may accumulate sufficient material from a companion, either through accretion or via a merger, to raise its core temperature, ignite carbon fusion, and trigger runaway nuclear fusion, completely disrupting the star. In the second case, the core of a massive star may undergo sudden gravitational collapse, releasing gravitational potential energy that can create a supernova explosion.The most recent directly observed supernova in the Milky Way was Kepler's Star of 1604 (SN 1604); remnants of two more recent supernovae have been found retrospectively. Observations in other galaxies indicate that supernovae should occur on average about three times every century in the Milky Way, and that any galactic supernova would almost certainly be observable in modern astronomical equipment. Supernovae play a significant role in enriching the interstellar medium with higher mass elements. Furthermore, the expanding shock waves from supernova explosions can trigger the formation of new stars.