Lecture 13 Main Sequence and Low Mass Evolution
... young as they only live for a few Million years. • You can’t tell how old an M dwarf is because their lives can be so long. • The Sun is ~ 5 Billion years old, so it will last only for ~ 5 Billion years longer. ...
... young as they only live for a few Million years. • You can’t tell how old an M dwarf is because their lives can be so long. • The Sun is ~ 5 Billion years old, so it will last only for ~ 5 Billion years longer. ...
Teresa Ashcraft
... evolutionary trend of the IRX and SSFR - IRX found from gas surface density and metallicity - metallicity grows with time - SFR determined by exponentially falling gas density The rise in the SFR density to z=1 is due to Galaxies in the mass range of the turnoff mass (10.5-11.5) Use IRX as a too ...
... evolutionary trend of the IRX and SSFR - IRX found from gas surface density and metallicity - metallicity grows with time - SFR determined by exponentially falling gas density The rise in the SFR density to z=1 is due to Galaxies in the mass range of the turnoff mass (10.5-11.5) Use IRX as a too ...
astro-ph/0502206 PDF
... b. Magnetic fields that penetrate the solar surface bring fast-moving, less-sorted, heavy ions (elements & isotopes) up from the interior of the Sun as the solar energetic particles (SEP) observed in violent solar flares and eruptions [8, 9]. c. Oxygen atoms are 33% heavier than Carbon atoms. The se ...
... b. Magnetic fields that penetrate the solar surface bring fast-moving, less-sorted, heavy ions (elements & isotopes) up from the interior of the Sun as the solar energetic particles (SEP) observed in violent solar flares and eruptions [8, 9]. c. Oxygen atoms are 33% heavier than Carbon atoms. The se ...
Chapter 13 White Dwarfs and Neutron Stars
... 13.2.3 Ingredients of a White Dwarf Description An initial description of a white dwarf may be afforded by a theory for which 1. The stable configurations correspond to hydrostatic equilibrium ...
... 13.2.3 Ingredients of a White Dwarf Description An initial description of a white dwarf may be afforded by a theory for which 1. The stable configurations correspond to hydrostatic equilibrium ...
Chapter 7
... To a surprising degree of accuracy we can assume that the Universe behaves adiabatically, i.e. during the expansion we can assume that all processes are reversible. And it also turns out that we can understand many of the thermal processes in the early universe with thermal equilibrium followed by “ ...
... To a surprising degree of accuracy we can assume that the Universe behaves adiabatically, i.e. during the expansion we can assume that all processes are reversible. And it also turns out that we can understand many of the thermal processes in the early universe with thermal equilibrium followed by “ ...
neutron star - Chabot College
... surface of a white dwarf in a binary system. In contrast, hydrogen fusion is steady on the surface of a neutron star in a binary system. However, the steady hydrogen burning builds up a layer of helium beneath the surface shell of hydrogen. Every few days, enough helium can build up for it to ignite ...
... surface of a white dwarf in a binary system. In contrast, hydrogen fusion is steady on the surface of a neutron star in a binary system. However, the steady hydrogen burning builds up a layer of helium beneath the surface shell of hydrogen. Every few days, enough helium can build up for it to ignite ...
pasta Jos´e A. Pons , Daniele Vigan`o and Nanda Rea
... It has long been hoped that stringent constraints could be placed on the equation of state of dense matter from astrophysical measurements of neutron stars, the compact remnants of the explosion of massive stars. Up to the present time, however, despite important breakthrough discoveries [1, 2, 3] ...
... It has long been hoped that stringent constraints could be placed on the equation of state of dense matter from astrophysical measurements of neutron stars, the compact remnants of the explosion of massive stars. Up to the present time, however, despite important breakthrough discoveries [1, 2, 3] ...
eng pdf 274 kb
... particle core and external nucleons bound into a cluster is typical not only of 6 Li nucleus, but also of 7 Li one. The obtained value of the cross section for coherent decay to an α particle and a triton, 27±4 mb, was found to be about the same as the cross section of paper [18] for 6 Li decay to α ...
... particle core and external nucleons bound into a cluster is typical not only of 6 Li nucleus, but also of 7 Li one. The obtained value of the cross section for coherent decay to an α particle and a triton, 27±4 mb, was found to be about the same as the cross section of paper [18] for 6 Li decay to α ...
MSci Astrophysics 210PHY412 - Queen's University Belfast
... The evolution of massive stars have the following general characteristics and differences to lower mass evolution 1. The electrons in their cores do not become degenerate until the final burning stages, when iron core is reached 2. Mass-loss plays an important role in the entire evolution (we will c ...
... The evolution of massive stars have the following general characteristics and differences to lower mass evolution 1. The electrons in their cores do not become degenerate until the final burning stages, when iron core is reached 2. Mass-loss plays an important role in the entire evolution (we will c ...
Gamma-Ray Line Emission from Radioactive Isotopes in Stars and
... Al in the Galaxy. Each prospective source has its advantages and difficulties. We discuss their nature briefly, addressing a few of the physical aspects involved. The treatment of convection, and its implications, constitute one problem area common to several source types. The convective coupling be ...
... Al in the Galaxy. Each prospective source has its advantages and difficulties. We discuss their nature briefly, addressing a few of the physical aspects involved. The treatment of convection, and its implications, constitute one problem area common to several source types. The convective coupling be ...
A0620-00 poster
... The orbital light curve of SS Cyg shows an ellipsoidal variation diluted by light from the disk and white dwarf. From an analysis of the ellipsoidal variations we limit the orbital inclination to the range 45° < i < 56°. The derived masses of the K star and white dwarf are MK = 0.55 ± 0.13 M and MW ...
... The orbital light curve of SS Cyg shows an ellipsoidal variation diluted by light from the disk and white dwarf. From an analysis of the ellipsoidal variations we limit the orbital inclination to the range 45° < i < 56°. The derived masses of the K star and white dwarf are MK = 0.55 ± 0.13 M and MW ...
Stars part 1
... 2. Luminosity – the total amount of energy a star radiates each second. Luminosity of all visible stars range from 1/1,000,000 the luminosity of the sun to 1,000,000 time the luminosity of the sun. 90% of the stars are not as bright as the sun. ...
... 2. Luminosity – the total amount of energy a star radiates each second. Luminosity of all visible stars range from 1/1,000,000 the luminosity of the sun to 1,000,000 time the luminosity of the sun. 90% of the stars are not as bright as the sun. ...
Stellar populations and dynamics in the Milky Way galaxy
... continued until the present. The ELS model was designed to provide conditions under which the oldest stars populated radially anisotropic orbits, while stars that formed later had increasingly circular orbits, in accordance with data which implied that the most metal-poor stars, assumed to be the ol ...
... continued until the present. The ELS model was designed to provide conditions under which the oldest stars populated radially anisotropic orbits, while stars that formed later had increasingly circular orbits, in accordance with data which implied that the most metal-poor stars, assumed to be the ol ...
black hole
... as much as 8 solar masses could lose mass fast enough to collapse to form white dwarfs with masses below 1.4 solar masses. ...
... as much as 8 solar masses could lose mass fast enough to collapse to form white dwarfs with masses below 1.4 solar masses. ...
Supplementary Information
... the limit of a thin and extended disk. The smearing due to the instrumental resolution in the spatial and spectral domains is taken into account by convolving the inclined model with the Gaussian point spread function of the appropriate width. The outputs of each model are full data cubes and veloci ...
... the limit of a thin and extended disk. The smearing due to the instrumental resolution in the spatial and spectral domains is taken into account by convolving the inclined model with the Gaussian point spread function of the appropriate width. The outputs of each model are full data cubes and veloci ...
Lecture 4
... Now: s = 1.35 = very big number => unique phenomenon! Happens very rarely! Measurements of s in the next decade confirm or reject this interpretation ...
... Now: s = 1.35 = very big number => unique phenomenon! Happens very rarely! Measurements of s in the next decade confirm or reject this interpretation ...
Thin-shell instability in collisionless plasma
... Earth’s magnetopause is probably the best-understood plasma shock [1,2]. Even larger shocks can form where energetic plasma outflows collide with the interstellar medium. The solar wind termination shock separates the heliosphere from the interstellar medium [3]. The existence of plasma shocks outsi ...
... Earth’s magnetopause is probably the best-understood plasma shock [1,2]. Even larger shocks can form where energetic plasma outflows collide with the interstellar medium. The solar wind termination shock separates the heliosphere from the interstellar medium [3]. The existence of plasma shocks outsi ...
Plasma Physics and Pulsars 2 - Max Planck Institut für
... by inverse beta decay in the continued neutronization of the core material during collapse. (The cross-section for the interaction of energetic neutrinos and nuclei at densities of 1012 gm/cm3 is sufficiently large as to trap the neutrinos by collisions in the imploding core. They are swept along wi ...
... by inverse beta decay in the continued neutronization of the core material during collapse. (The cross-section for the interaction of energetic neutrinos and nuclei at densities of 1012 gm/cm3 is sufficiently large as to trap the neutrinos by collisions in the imploding core. They are swept along wi ...
Dark Stars: Dark Matter Annihilation in the First Stars.
... • Even once the first stars reach the main sequence, DM annihilation can still be very important. – DM Can again be the dominant heat source. – DM heating may also determine the mass of the first stars. ...
... • Even once the first stars reach the main sequence, DM annihilation can still be very important. – DM Can again be the dominant heat source. – DM heating may also determine the mass of the first stars. ...
PowerPoint Presentation - Neutron stars, pulsars and black
... • The discovery of pulsars that were spinning more than 100 times per second (the first was spinning 640 times per second) threw the field for a loop. When some millisecond pulsars were discovered in old star clusters it was even more confusing. • Eventually it was determined that all millisecond pu ...
... • The discovery of pulsars that were spinning more than 100 times per second (the first was spinning 640 times per second) threw the field for a loop. When some millisecond pulsars were discovered in old star clusters it was even more confusing. • Eventually it was determined that all millisecond pu ...
Astrophysics
... numerical tools that can be used to investigate these strongly gravitating systems and predict the gravitational radiation emitted by SNe and GRBs. Prof. Lazzati studies the theory of long-duration GRBs, believed to be produced by relativistic jets of plasma ejected in the core of massive stars at t ...
... numerical tools that can be used to investigate these strongly gravitating systems and predict the gravitational radiation emitted by SNe and GRBs. Prof. Lazzati studies the theory of long-duration GRBs, believed to be produced by relativistic jets of plasma ejected in the core of massive stars at t ...
P-nuclei
p-Nuclei (p stands for proton-rich) are certain proton-rich, naturally occurring isotopes of some elements between selenium and mercury which cannot be produced in either s- or r-process.