News from high-mass twin stars
... The pomerons (wavy lines) couple to different quarks (solid lines) in quark matter (as in the hNJL Lagrangian) or to quarks in different baryons in nuclear matter (giving rise to repulsive 3- and 4- body interactions). ...
... The pomerons (wavy lines) couple to different quarks (solid lines) in quark matter (as in the hNJL Lagrangian) or to quarks in different baryons in nuclear matter (giving rise to repulsive 3- and 4- body interactions). ...
PPT Slides - Center for Computational Sciences
... • Gas collapses under its own gravity • Densities build up until fusion starts in the center. ...
... • Gas collapses under its own gravity • Densities build up until fusion starts in the center. ...
Export To Word
... diagram will likely benefit from working on the questions first. These questions should also be used as guidelines to help the students write their response letters. (91-110 min.) Collect and Review Collect all of the completed work and other materials from each group (H-R Diagram, Response Letter ...
... diagram will likely benefit from working on the questions first. These questions should also be used as guidelines to help the students write their response letters. (91-110 min.) Collect and Review Collect all of the completed work and other materials from each group (H-R Diagram, Response Letter ...
What is the biggest star? - University of Central Lancashire
... In star formation, the gravitational energy is balanced by energy from pressure from the gas cloud itself, but if the cloud is big enough the gravitational energy becomes larger than the pressure so gravity pulls the cloud inward which eventually forms a star. How can stars ignite when there isn’t a ...
... In star formation, the gravitational energy is balanced by energy from pressure from the gas cloud itself, but if the cloud is big enough the gravitational energy becomes larger than the pressure so gravity pulls the cloud inward which eventually forms a star. How can stars ignite when there isn’t a ...
Chapter 10 Late evolution of low- and intermediate
... outer envelope) starts expanding in response to core contraction. A fairly long-lived phase follows in which the stellar luminosity is provided almost entirely by He-shell burning (phase H-K in Fig. 10.1). This is called the early AGB phase. The He-burning shell gradually adds mass to the growing CO ...
... outer envelope) starts expanding in response to core contraction. A fairly long-lived phase follows in which the stellar luminosity is provided almost entirely by He-shell burning (phase H-K in Fig. 10.1). This is called the early AGB phase. The He-burning shell gradually adds mass to the growing CO ...
File - Physics with Mr. Mason
... brightness and temperature of stars were related. You are going to make a Hertzsprung-Russell diagram from the data given at the back of this booklet. Take note of the following The axes on a HR diagram are kind of backwards. Use the axes given and be careful when plotting points! Most stars are ...
... brightness and temperature of stars were related. You are going to make a Hertzsprung-Russell diagram from the data given at the back of this booklet. Take note of the following The axes on a HR diagram are kind of backwards. Use the axes given and be careful when plotting points! Most stars are ...
Project 9: Stellar Spectra: Temperature
... strengths of the absorption lines and therefore calculate the chemical composition of the outer part of a star. Relative absorption line strengths can also be used to find temperatures and densities. Absorption lines occur when an electron absorbs energy from the spectrum to move up the ...
... strengths of the absorption lines and therefore calculate the chemical composition of the outer part of a star. Relative absorption line strengths can also be used to find temperatures and densities. Absorption lines occur when an electron absorbs energy from the spectrum to move up the ...
Death - Wayne State University Physics and Astronomy
... the protons and electrons fuse together to form neutrons and neutrinos • The core, once the size of the Earth, becomes a very stiff neutron star about the size of a small town in less than a second • The in falling outer layers hit the core and heat up to billions of degrees from the impact 12 April ...
... the protons and electrons fuse together to form neutrons and neutrinos • The core, once the size of the Earth, becomes a very stiff neutron star about the size of a small town in less than a second • The in falling outer layers hit the core and heat up to billions of degrees from the impact 12 April ...
Chapter 9 Post-main sequence evolution through helium burning
... the luminosity increases as the effective temperature remains at the approximately constant value corresponding to the Hayashi line. The expansion of the star between D and E still occurs on the thermal timescale, so the H-shell burning phase of intermediate-mass stars on the red-giant branch is ver ...
... the luminosity increases as the effective temperature remains at the approximately constant value corresponding to the Hayashi line. The expansion of the star between D and E still occurs on the thermal timescale, so the H-shell burning phase of intermediate-mass stars on the red-giant branch is ver ...
Adiabatic evolution of mass-losing stars
... might continue to burn for a short time but this will not change the evolution of the structure, as long as mass-loss time-scale is much shorter than the thermal time-scale.) In our EMRI binary system, the star is assumed to be in a circular, equatorial orbit around the central supermassive black ho ...
... might continue to burn for a short time but this will not change the evolution of the structure, as long as mass-loss time-scale is much shorter than the thermal time-scale.) In our EMRI binary system, the star is assumed to be in a circular, equatorial orbit around the central supermassive black ho ...
A new class of rapidly pulsating star
... there is a substantial Balmer jump observed in PB 8783. In order to include this extra information in the fitting, Planck functions were replaced by model atmospheres from Kurucz (1992) to represent Sl (Tl> v) and Sz(Tz, v). For the red star logg=4 models were used, while for the blue star logg=5 mo ...
... there is a substantial Balmer jump observed in PB 8783. In order to include this extra information in the fitting, Planck functions were replaced by model atmospheres from Kurucz (1992) to represent Sl (Tl> v) and Sz(Tz, v). For the red star logg=4 models were used, while for the blue star logg=5 mo ...
Stellar Atmospheres
... Collisional rates are proportional to the particle density – in high densities departures from LTE will be small. Deep in the atmosphere photons do not escape and intensity is close to the equilibrium value – departures from LTE are small even if the radiative rates dominate over the collisional rat ...
... Collisional rates are proportional to the particle density – in high densities departures from LTE will be small. Deep in the atmosphere photons do not escape and intensity is close to the equilibrium value – departures from LTE are small even if the radiative rates dominate over the collisional rat ...
Which Stars Form Black Holes and Neutron Stars?
... are associated with radio pulsars or X-ray emitting central compact objects [37]. The second method is to generate scenarios through which HMXBs could have formed. More massive stars end their lives first, so one would tend to expect that the mass of the mass donor in the binary would represent a l ...
... are associated with radio pulsars or X-ray emitting central compact objects [37]. The second method is to generate scenarios through which HMXBs could have formed. More massive stars end their lives first, so one would tend to expect that the mass of the mass donor in the binary would represent a l ...
FIRST LIGHT IN THE UNIVERSE
... Myr with large dust opacity (sub-mm galaxy overlap) • Superwinds drive out both gas and dust, resulting in more quiescent star formation (10’s M yr-1) and smaller UV extinction • Quiescent star formation phase lasts for at least a few hundred Myr; by end at least a few 1010 M of stars have formed ...
... Myr with large dust opacity (sub-mm galaxy overlap) • Superwinds drive out both gas and dust, resulting in more quiescent star formation (10’s M yr-1) and smaller UV extinction • Quiescent star formation phase lasts for at least a few hundred Myr; by end at least a few 1010 M of stars have formed ...
Galaxy Formation,! Reionization, ! the First Stars and Quasars! Ay 127!
... • The early stages of galaxy evolution - but there is no clear-cut boundary, and it also has two principal aspects: assembly of the mass, and conversion of gas into stars! • Must be related to large-scale (hierarchical) structure formation, plus the dissipative processes - it is a very messy proce ...
... • The early stages of galaxy evolution - but there is no clear-cut boundary, and it also has two principal aspects: assembly of the mass, and conversion of gas into stars! • Must be related to large-scale (hierarchical) structure formation, plus the dissipative processes - it is a very messy proce ...
Presentazione di PowerPoint
... populations with new eyes. De facto, a new era on globular cluster research is started: 1) Many serious problems remain unsolved, and we still have a rather incoherent picture. The new HST cameras that will be available after SM4 will play a main role in composing the puzzle. 2) For the first time, ...
... populations with new eyes. De facto, a new era on globular cluster research is started: 1) Many serious problems remain unsolved, and we still have a rather incoherent picture. The new HST cameras that will be available after SM4 will play a main role in composing the puzzle. 2) For the first time, ...
Spectroscopy – Lecture 1
... This is the cross section in square cm per H atom for the fraction of the electrons in the velocity interval v to v + dv. To get complete f-f absorption must integrate over v. ...
... This is the cross section in square cm per H atom for the fraction of the electrons in the velocity interval v to v + dv. To get complete f-f absorption must integrate over v. ...
Kinematics of the Solar Neighborhood
... In practice the velocity ellipsoid for a given ensemble of stars (e.g. all stars of a given stellar type) is never prefectly diagonalized. The most significant term to be added to (15.13) is proportional to u(v − va ), indicating that the velocity ellipsoid lies in the plane of the disk, but is not ...
... In practice the velocity ellipsoid for a given ensemble of stars (e.g. all stars of a given stellar type) is never prefectly diagonalized. The most significant term to be added to (15.13) is proportional to u(v − va ), indicating that the velocity ellipsoid lies in the plane of the disk, but is not ...
Fe I/Fe II ionization equilibrium in cool stars: NLTE versus LTE
... In all previous NLTE calculations, the model atom of Fe I was build using measured energy levels. The experimental analysis of Nave et al. (1994) with later updates provided 965 energy levels for Fe I. A comparison with the calculated Fe I atomic structure (Kurucz (2007)) reveals that the system of ...
... In all previous NLTE calculations, the model atom of Fe I was build using measured energy levels. The experimental analysis of Nave et al. (1994) with later updates provided 965 energy levels for Fe I. A comparison with the calculated Fe I atomic structure (Kurucz (2007)) reveals that the system of ...
Where Do Baby Stars Come From?
... Other neat things are also going on. This giant cloud has all sorts of gravitational potential energy in it. The atoms are spread out across space, but there’s a central point to the space. As things move inwards toward that central point, gravitational energy gets converted to kinetic energy. The p ...
... Other neat things are also going on. This giant cloud has all sorts of gravitational potential energy in it. The atoms are spread out across space, but there’s a central point to the space. As things move inwards toward that central point, gravitational energy gets converted to kinetic energy. The p ...
The Galactic Halo
... Stars with enhanced abundances of carbon (CEMP stars), and other light elements (including the lowest [Fe/H] star yet discovered), and lack of over-abundances of neutron-capture elements (CEMP-no stars) Associated with production by “faint SNe” – progenitors with mass on the order of 10-100 Mo under ...
... Stars with enhanced abundances of carbon (CEMP stars), and other light elements (including the lowest [Fe/H] star yet discovered), and lack of over-abundances of neutron-capture elements (CEMP-no stars) Associated with production by “faint SNe” – progenitors with mass on the order of 10-100 Mo under ...
The origin of magnetism on the upper main sequence
... to concentrate on the low-mass end of the stellar mass spectrum. This is so even in the most recent computations (Bate 2009b) where some account is taken of radiative feedback, which will be of much greater importance in the process of the formation of more massive stars (Krumholtz 2006). Computatio ...
... to concentrate on the low-mass end of the stellar mass spectrum. This is so even in the most recent computations (Bate 2009b) where some account is taken of radiative feedback, which will be of much greater importance in the process of the formation of more massive stars (Krumholtz 2006). Computatio ...
Lecture20
... helium, it has an energy crisis Because the star is small, it cannot ignite the remaining material in its core and so the star collapses and forms a ...
... helium, it has an energy crisis Because the star is small, it cannot ignite the remaining material in its core and so the star collapses and forms a ...
How do we know what stars are
... appear in the spectrum. Heavier and heavier elements will be formed as the core runs out of hydrogen and helium. Stars cannot fuse atoms larger than the element __________. Toward the end of the life of the star, the fusion reaction no longer produces enough outward force to balance its own _______. ...
... appear in the spectrum. Heavier and heavier elements will be formed as the core runs out of hydrogen and helium. Stars cannot fuse atoms larger than the element __________. Toward the end of the life of the star, the fusion reaction no longer produces enough outward force to balance its own _______. ...