Effects of color superconductivity on the nucleation of
... hadronic compact stars with respect to the conversion to quark stars using different relativistic models for the EoS: Non Linear Walecka Model (NLWM) & Quark Meson Coupling (QMC). We have explored the effect of different hyperon couplings on the critical mass and on the stellar conversion energy, fi ...
... hadronic compact stars with respect to the conversion to quark stars using different relativistic models for the EoS: Non Linear Walecka Model (NLWM) & Quark Meson Coupling (QMC). We have explored the effect of different hyperon couplings on the critical mass and on the stellar conversion energy, fi ...
A neutron star with a carbon atmosphere in the Cassiopeia A
... The efficient separation of light and heavy elements results in atmospheres composed of a single element.25 The opacities are obtained from tables computed by the Opacity Project.26 (The energy range of the tables covers E/kT ∼ 0.07 − 20. When opacities are required beyond this range, we use the E − ...
... The efficient separation of light and heavy elements results in atmospheres composed of a single element.25 The opacities are obtained from tables computed by the Opacity Project.26 (The energy range of the tables covers E/kT ∼ 0.07 − 20. When opacities are required beyond this range, we use the E − ...
Available online www.jsaer.com Journal of Scientific and
... Turbulence deep within these clouds gives rise to knots with sufficient mass that the gas and dust can begin to collapse under its own gravitational attraction. As the cloud collapses, the material at the centre begins to heat up. This is known as a protostar, it is this hot core at the heart of the ...
... Turbulence deep within these clouds gives rise to knots with sufficient mass that the gas and dust can begin to collapse under its own gravitational attraction. As the cloud collapses, the material at the centre begins to heat up. This is known as a protostar, it is this hot core at the heart of the ...
Evolution of supermassive stars as a pathway to black hole formation
... Such models, however, beg the question of how a supermassive star might realistically form. Creating a 106 M⊙ star requires the very rapid accumulation of gas. Since the thermonuclear timescale for a star burning hydrogen at the Eddington limit is ∼ 2 Myr, independent of mass, and will be less if on ...
... Such models, however, beg the question of how a supermassive star might realistically form. Creating a 106 M⊙ star requires the very rapid accumulation of gas. Since the thermonuclear timescale for a star burning hydrogen at the Eddington limit is ∼ 2 Myr, independent of mass, and will be less if on ...
The accretion properties of the intermediate mass Herbig Ae/Be stars
... Aim is to find more about the intermediate mass stars – no follow-on studies since 1999 ...
... Aim is to find more about the intermediate mass stars – no follow-on studies since 1999 ...
Supernovae and compact objects
... very closely in a binary system. If they are sufficiently close, they will emit gravitational radiation as they orbit, which will remove energy from the orbit and cause them to eventually collide and merge. This is referred to as the double-degenerate scenario, since it involves two degenerate stars ...
... very closely in a binary system. If they are sufficiently close, they will emit gravitational radiation as they orbit, which will remove energy from the orbit and cause them to eventually collide and merge. This is referred to as the double-degenerate scenario, since it involves two degenerate stars ...
main sequence stars of a open cluster
... You will photometry about 100 stars for both N1912Bs.fits and N1912Vs.fits. Adjust the viewing so that you can see faint stars as well. Magnifying by two may help you work easily. Find Zoom up icon in the upper left of the Makali`i window; it has a picture of magnifier with a plus mark. Clicking onc ...
... You will photometry about 100 stars for both N1912Bs.fits and N1912Vs.fits. Adjust the viewing so that you can see faint stars as well. Magnifying by two may help you work easily. Find Zoom up icon in the upper left of the Makali`i window; it has a picture of magnifier with a plus mark. Clicking onc ...
Presentazione di PowerPoint
... and gas is predominantly Keplerian (relativistic effects are minimal), with a component due to the combined gravitational potential of stars, dust, gas, dark matter, and anything else contributing mass to within that region. Beyond the sphere of influence, the gravitational dominance of the SMBH qui ...
... and gas is predominantly Keplerian (relativistic effects are minimal), with a component due to the combined gravitational potential of stars, dust, gas, dark matter, and anything else contributing mass to within that region. Beyond the sphere of influence, the gravitational dominance of the SMBH qui ...
PDF Format
... W-type class: W-type systems are generally composed of stars of later spectral type (from F to K). In the W-type W UMa stars, the deeper primary minimum corresponds to the occultation eclipse of the smaller, less massive component. Stars in the W-type systems are generally closer to the zero age mai ...
... W-type class: W-type systems are generally composed of stars of later spectral type (from F to K). In the W-type W UMa stars, the deeper primary minimum corresponds to the occultation eclipse of the smaller, less massive component. Stars in the W-type systems are generally closer to the zero age mai ...
Does Transparent Hidden Matter Generate Optical Scintillation?
... • Average mass column density towards LMC 250g/m2 or a column of 3m H2 (normal P and T) Clouds cover 1% of sky => concentration of 100 ...
... • Average mass column density towards LMC 250g/m2 or a column of 3m H2 (normal P and T) Clouds cover 1% of sky => concentration of 100 ...
The AcroCoRoT objectives (10 min) - IAG-Usp
... AcRoCorot objectives : be ready when data come to use them efficiently hence organisation of meetings such as the present one to motivate - teams with similar interest to continue to meet and talk (collaboration, exchange of brain thinkings and tools) ...
... AcRoCorot objectives : be ready when data come to use them efficiently hence organisation of meetings such as the present one to motivate - teams with similar interest to continue to meet and talk (collaboration, exchange of brain thinkings and tools) ...
Lecture3
... Measure brightness b, take brightness ratio bB / bU; bV / bB gives color •Photometry measures the apparent brightness of a ...
... Measure brightness b, take brightness ratio bB / bU; bV / bB gives color •Photometry measures the apparent brightness of a ...
Head-On Collision of Neutron Stars As A Thought Experiment
... Following the head-on collision of the two neutron stars, two recoil shocks form at the point of contact and propagate back into each star along the collision axis. Matter passing through the shock is heated and decelerated, as its kinetic energy is converted into thermal energy. The configuration i ...
... Following the head-on collision of the two neutron stars, two recoil shocks form at the point of contact and propagate back into each star along the collision axis. Matter passing through the shock is heated and decelerated, as its kinetic energy is converted into thermal energy. The configuration i ...
Kathy Geise `08 - DU Portfolio
... Stellar Atmospheres: A Computational Approach developing stellar atmosphere models because the software met each of the four criteria and because the advisor team had many years of experience using IDL. In the end, three separate stellar atmosphere models were developed to answer questions posed by ...
... Stellar Atmospheres: A Computational Approach developing stellar atmosphere models because the software met each of the four criteria and because the advisor team had many years of experience using IDL. In the end, three separate stellar atmosphere models were developed to answer questions posed by ...
ESO telescopes
... combination instrument AMBER15, we combined the light of three of the VLTI 1.8 m telescopes and measured the interferometric observables (visibilities and closure phases) in 17 spectral channels in the K band (λ=1.95–2.55 μm). The VLTI observations were obtained using three different telescope tripl ...
... combination instrument AMBER15, we combined the light of three of the VLTI 1.8 m telescopes and measured the interferometric observables (visibilities and closure phases) in 17 spectral channels in the K band (λ=1.95–2.55 μm). The VLTI observations were obtained using three different telescope tripl ...
Presentation (PowerPoint File)
... Equation of state: isothermal or barotropic above 10^-14 g cm-3 Isothermal collapse results in many small fragments; barotropic collapse in a few. In no case did a massive star form (although simulation ran only until ~ 10% of mass had gone into stars). Require radiation-hydrodynamic simulations to ...
... Equation of state: isothermal or barotropic above 10^-14 g cm-3 Isothermal collapse results in many small fragments; barotropic collapse in a few. In no case did a massive star form (although simulation ran only until ~ 10% of mass had gone into stars). Require radiation-hydrodynamic simulations to ...
General Module information
... Draw an HR diagram and properly label its axes with appropriate units. Sketch the following regions of interest on an HR diagram: – The main sequence – The red giant branch – White dwarfs – The turn-off point – The horizontal branch – The instability strip (refer to Variable Stars, below) Explain wh ...
... Draw an HR diagram and properly label its axes with appropriate units. Sketch the following regions of interest on an HR diagram: – The main sequence – The red giant branch – White dwarfs – The turn-off point – The horizontal branch – The instability strip (refer to Variable Stars, below) Explain wh ...
Astronomy 110 Announcements: Life and Death of a Low Mass Star
... Stage #6: White Dwarf The central remaining core is very hot, leading to ionization of the surrounding gas shell. ...
... Stage #6: White Dwarf The central remaining core is very hot, leading to ionization of the surrounding gas shell. ...
The Primordial Abundance of $^ 6$ Li and $^ 9$ be
... Teff = 6090 ± 100 K. This is ∼ 100 K lower than other estimates for this star. For example, Thorburn (1994) determined an effective temperature of 6232 ± 100 K for this star. King (1993) advocates a higher temperature scale for halo stars, and finds Teff = 6312. We will assume that the effective tem ...
... Teff = 6090 ± 100 K. This is ∼ 100 K lower than other estimates for this star. For example, Thorburn (1994) determined an effective temperature of 6232 ± 100 K for this star. King (1993) advocates a higher temperature scale for halo stars, and finds Teff = 6312. We will assume that the effective tem ...
ppt
... • In general it is not possible to uncover the inclination angle. However, for large samples of a given type of star it may be appropriate to take the average inclination to determine the ...
... • In general it is not possible to uncover the inclination angle. However, for large samples of a given type of star it may be appropriate to take the average inclination to determine the ...
Sporadic Mass Ejection in Red Supergiants
... For a working model, we postulate the existence of turbulent elements of scale size s ""' 5% of the stellar radius R; this corresponds to approximately 1600 elements. If the characteristic velocity Vrms,....., 30 km s- 1, consistent with late type supergiant spectra, then approximately 3% of the ele ...
... For a working model, we postulate the existence of turbulent elements of scale size s ""' 5% of the stellar radius R; this corresponds to approximately 1600 elements. If the characteristic velocity Vrms,....., 30 km s- 1, consistent with late type supergiant spectra, then approximately 3% of the ele ...
Interactive 4 - Hertzsprung-Russell Diagram Explorer
... Check the “Auto” box in the speed section then click “Create Star”. Check “Show Regions” to display regions where the main sequence stars and the giants are located. Once the animation is complete, click on any part of the star’s evolutionary path on the H-R diagram to see the size, colour and the s ...
... Check the “Auto” box in the speed section then click “Create Star”. Check “Show Regions” to display regions where the main sequence stars and the giants are located. Once the animation is complete, click on any part of the star’s evolutionary path on the H-R diagram to see the size, colour and the s ...
Physics of Galaxies 2016 Exercises with solutions – Batch II
... gas surrounding young, hot stars. However, such stars are short-lived, and as soon as they start to die off, the Hα luminosity drops. The continuum beneath the line has two different components: 1. nebular continuum from the photoionized gas. At these wavelengths, it’s main free-bound processes; at ...
... gas surrounding young, hot stars. However, such stars are short-lived, and as soon as they start to die off, the Hα luminosity drops. The continuum beneath the line has two different components: 1. nebular continuum from the photoionized gas. At these wavelengths, it’s main free-bound processes; at ...
Lokal fulltext - Chalmers Publication Library
... ejected by the star affects the shape and evolution of the future supernova remnant, and how the material is incorporated into the interstellar medium. Over time, these processes affect the chemical evolution of the interstellar medium on a galactic scale. This thesis probes these topics at differen ...
... ejected by the star affects the shape and evolution of the future supernova remnant, and how the material is incorporated into the interstellar medium. Over time, these processes affect the chemical evolution of the interstellar medium on a galactic scale. This thesis probes these topics at differen ...