Stellar capture by an accretion disc
... mass and angular momentum between the star and the disc, and also to determine how star–disc interactions influence the distribution of stellar orbits near a massive central object. An important and difficult task is to estimate the probability that a star is captured from an originally unbound orbi ...
... mass and angular momentum between the star and the disc, and also to determine how star–disc interactions influence the distribution of stellar orbits near a massive central object. An important and difficult task is to estimate the probability that a star is captured from an originally unbound orbi ...
Shear Stress Transmission Model for the Flagellar Rotary Motor
... the y-z plane. Then the proton passage in the channel will give Rotor a torque if the surface of Rotor has a suitable charge distribution. This model, however, did not explain the experimental data and was discarded. Then, it is assumed that the proton channel is perpendicular to the membrane as sho ...
... the y-z plane. Then the proton passage in the channel will give Rotor a torque if the surface of Rotor has a suitable charge distribution. This model, however, did not explain the experimental data and was discarded. Then, it is assumed that the proton channel is perpendicular to the membrane as sho ...
P Cygni Profiles of Molecular Lines Toward Arp 220 Nuclei
... 2005), as well as models of HCO+ enhancement in protostellar outflow shocks (Rawlings et al. 2004). The absorbing gas will have a depth on the order of 1–10 pc if its density is at the CO(3–2) critical density of 104 cm−3 . The actual absorbing material can be distributed over a longer length if it ...
... 2005), as well as models of HCO+ enhancement in protostellar outflow shocks (Rawlings et al. 2004). The absorbing gas will have a depth on the order of 1–10 pc if its density is at the CO(3–2) critical density of 104 cm−3 . The actual absorbing material can be distributed over a longer length if it ...
Non-spherical core collapse supernovae-I. Neutrino
... only the innermost stellar core needs to be resolved adequately. In contrast, in the second, hydrodynamic part, the physics of the problem simplifies to the solution of the hydrodynamic equations because (to a good approximation) the central neutron star influences the dynamics of the ejecta only vi ...
... only the innermost stellar core needs to be resolved adequately. In contrast, in the second, hydrodynamic part, the physics of the problem simplifies to the solution of the hydrodynamic equations because (to a good approximation) the central neutron star influences the dynamics of the ejecta only vi ...
Detached WD/BD binaries as progenitors of CVs
... • PHL5038 is flagged as partially resolved in UKIDSS • From evolutionary considerations, WD+BD binaries should either be wide (> few AU) or close (post-CE) – Substellar companion either spirals inwards in CE, or orbit expands outwards as Red Giant loses mass – Farihi, Hoard & Wachter (2006) ...
... • PHL5038 is flagged as partially resolved in UKIDSS • From evolutionary considerations, WD+BD binaries should either be wide (> few AU) or close (post-CE) – Substellar companion either spirals inwards in CE, or orbit expands outwards as Red Giant loses mass – Farihi, Hoard & Wachter (2006) ...
MEASURING THE STARS
... The magnitude system Stellar surface temperature The spectral classificaGon of stars Hertzprung-‐Russel Diagram Stellar Luminosity Classes Stellar Radii ...
... The magnitude system Stellar surface temperature The spectral classificaGon of stars Hertzprung-‐Russel Diagram Stellar Luminosity Classes Stellar Radii ...
ppt - chris.engelbrecht.nithep.ac.za
... Nucleosynthesis: Probing the Progenitor Core Kifonidis et al. 2000 ...
... Nucleosynthesis: Probing the Progenitor Core Kifonidis et al. 2000 ...
Rotational effects on the oscillation frequencies of newly born proto
... extensively been studied in recent years after Andersson (1998) pointed out that it is generic for every rotating star, and since the coupling of the r–mode with the current multipoles is strong, it was proposed that this instability plays an important role in nascent neutron stars. In principle, al ...
... extensively been studied in recent years after Andersson (1998) pointed out that it is generic for every rotating star, and since the coupling of the r–mode with the current multipoles is strong, it was proposed that this instability plays an important role in nascent neutron stars. In principle, al ...
Carbon Enhanced Stars in the Sloan Digital Sky Survey ( SDSS )
... HE 0007-1832 Cohen et al 2004 12C/13C ~ 6 – 9 (CNO equilibrium) Also have slightly higher nitrogen abundance compared to s-process rich stars. ...
... HE 0007-1832 Cohen et al 2004 12C/13C ~ 6 – 9 (CNO equilibrium) Also have slightly higher nitrogen abundance compared to s-process rich stars. ...
Subatomic Physics: the Notes - McMaster Physics and Astronomy
... By this time the electric charge of the electron had been measured (through the Millikan oil-drop experiment of 1909) and so it was known that the electron had a charge equal in size to (but opposite in sign from) the charge, q = e, of the Hydrogen ion (what we now call the Hydrogen nucleus, or pro ...
... By this time the electric charge of the electron had been measured (through the Millikan oil-drop experiment of 1909) and so it was known that the electron had a charge equal in size to (but opposite in sign from) the charge, q = e, of the Hydrogen ion (what we now call the Hydrogen nucleus, or pro ...
(r) and
... It can be shown easily that any integral of motion, or any function which depends on (x,v,t) only through an integral of motion, is a solution of the time dependent CBE. Again, let’s limit ourselves to time-independent systems. ...
... It can be shown easily that any integral of motion, or any function which depends on (x,v,t) only through an integral of motion, is a solution of the time dependent CBE. Again, let’s limit ourselves to time-independent systems. ...
Delta isobars in neutron stars
... Λ which are the most relevant heavy baryons in beta stable matter. The continuous lines correspond to the case of universal couplings while the dashed lines to the case in which xωΔ is suppressed with respect to xσΔ as indicated by the scattering data. In the most unfavorable case for deltas, i.e. x ...
... Λ which are the most relevant heavy baryons in beta stable matter. The continuous lines correspond to the case of universal couplings while the dashed lines to the case in which xωΔ is suppressed with respect to xσΔ as indicated by the scattering data. In the most unfavorable case for deltas, i.e. x ...
The AcroCoRoT objectives (10 min) - IAG-Usp
... 2nd CoRoT Brazil Workshop Ubatuba, November 2005 ...
... 2nd CoRoT Brazil Workshop Ubatuba, November 2005 ...
Testing - uwyo.edu
... end in supernova explosions. • Low-mass stars with < 2MSun have long lives, never become hot enough to fuse carbon nuclei, and end as white dwarfs. • Intermediate-mass stars can make elements heavier than carbon but end as white dwarfs. © 2010 Pearson Education, Inc. ...
... end in supernova explosions. • Low-mass stars with < 2MSun have long lives, never become hot enough to fuse carbon nuclei, and end as white dwarfs. • Intermediate-mass stars can make elements heavier than carbon but end as white dwarfs. © 2010 Pearson Education, Inc. ...
UNIFYING THEORY OF LOW-ENERGY NUCLEAR REACTION AND
... indicate also that the deuteron-lithium (D+Li) fusion rate, and the proton-boron (p+B) fusion rate and the proton-lithium (p + Li) fusion rate in a metal/alloy at ambient temperatures are also substantially enhanced due to this quantum plasma nuclear fusion (QPNF) mechanism. Implications of our resu ...
... indicate also that the deuteron-lithium (D+Li) fusion rate, and the proton-boron (p+B) fusion rate and the proton-lithium (p + Li) fusion rate in a metal/alloy at ambient temperatures are also substantially enhanced due to this quantum plasma nuclear fusion (QPNF) mechanism. Implications of our resu ...
Double Layer Observations and role in particle acceleration
... Double layers are regions of charge separation along B that produce parallel E and parallel potential drops They were proposed by Alfven 55 years ago to be the mechanism for accelerating electrons in astrophysics Until now, they have not been observed with sufficient total potentials to matter VAP h ...
... Double layers are regions of charge separation along B that produce parallel E and parallel potential drops They were proposed by Alfven 55 years ago to be the mechanism for accelerating electrons in astrophysics Until now, they have not been observed with sufficient total potentials to matter VAP h ...
The coupling between the core/cusp and missing satellite problems
... centrally-divergent DM cusps on scales relevant to observations of dwarf spheroidal galaxies (dSphs). We estimate that the CDM haloes often associated with the Milky Way’s dSphs (Mvir /M⊙ ∼ 109−10 ) require ∆E ∼ 1053−55 erg in order to form cores on scales comparable to the luminous size of these ga ...
... centrally-divergent DM cusps on scales relevant to observations of dwarf spheroidal galaxies (dSphs). We estimate that the CDM haloes often associated with the Milky Way’s dSphs (Mvir /M⊙ ∼ 109−10 ) require ∆E ∼ 1053−55 erg in order to form cores on scales comparable to the luminous size of these ga ...
San Diego Astronomy Association CONTENTS
... ly the carbon core of sun sized stars which have exhausted their hydrogen and helium fuels and released their outer atmospheres as planetary nebula. The carbon cores emerge from the planetary nebula as white-hot remnants unable to support further nuclear fusion and slowly cool over billions of years ...
... ly the carbon core of sun sized stars which have exhausted their hydrogen and helium fuels and released their outer atmospheres as planetary nebula. The carbon cores emerge from the planetary nebula as white-hot remnants unable to support further nuclear fusion and slowly cool over billions of years ...
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.