Stellar Relaxation Times
... respect to the surrounding stars. A density of ~ 1 star pc-3, then implies a relaxation time of ~ 1014 yr. The Sun’s orbit about the center of the Galaxy is not gravitationally affected by other stars. On the other hand, giant molecular clouds have masses that are ~ 108 M. Although the number densi ...
... respect to the surrounding stars. A density of ~ 1 star pc-3, then implies a relaxation time of ~ 1014 yr. The Sun’s orbit about the center of the Galaxy is not gravitationally affected by other stars. On the other hand, giant molecular clouds have masses that are ~ 108 M. Although the number densi ...
High temperature reaction kinetics of CN(v = 0) with C2H4 and
... in the outer shells except if shocks, induced by pulsations of the star, end up playing a major role there. In Ori(KL), astronomical observations show that the vibrational energy distribution of HCN departs from MaxwellBoltzmann equilibrium because of infrared pumping [16]. Back in the laboratory, a ...
... in the outer shells except if shocks, induced by pulsations of the star, end up playing a major role there. In Ori(KL), astronomical observations show that the vibrational energy distribution of HCN departs from MaxwellBoltzmann equilibrium because of infrared pumping [16]. Back in the laboratory, a ...
Electromagnetic Properties of Neutrinos
... and experimental constraints on the neutrino charge radius. In Section 5, we discuss neutrino radiative decay and the astrophysical bounds on a neutrino magnetic moment obtained from the study of plasmon decay in stars. In Section 6 we discuss neutrino spin and spin-flavor precession. In conclusion, ...
... and experimental constraints on the neutrino charge radius. In Section 5, we discuss neutrino radiative decay and the astrophysical bounds on a neutrino magnetic moment obtained from the study of plasmon decay in stars. In Section 6 we discuss neutrino spin and spin-flavor precession. In conclusion, ...
Calculations of Gamma Ray Dose from Gamma Ray Bursters and
... Gamma ray bursters (GRB) were first identified over 30 years ago but their origin was unknown until very recently. There is a growing consensus that they are the result of extremely high-energy supernovae events that have been dubbed “GRB” and they can be detected at cosmological distances, but many ...
... Gamma ray bursters (GRB) were first identified over 30 years ago but their origin was unknown until very recently. There is a growing consensus that they are the result of extremely high-energy supernovae events that have been dubbed “GRB” and they can be detected at cosmological distances, but many ...
Metallicity, Age, and Mass of Star Forming Galaxies at z~3
... Clustering of mass cannot have grown to such an extent at z~3 in “reasonable” cosmologies Bias: galaxies form in biased regions of the mass distribution In principle, it can constrain the mass spectrum ...
... Clustering of mass cannot have grown to such an extent at z~3 in “reasonable” cosmologies Bias: galaxies form in biased regions of the mass distribution In principle, it can constrain the mass spectrum ...
extrasolar planets
... – Reflected light (visible wavelengths) of the planet is extremely faint: factor of ~1 billion – Emitted light (infrared wavelengths) of the planet is still very faint: factor of ~1 million • Imaging of planets around Sun-like stars is currently not possible. Several ground-based and space- ...
... – Reflected light (visible wavelengths) of the planet is extremely faint: factor of ~1 billion – Emitted light (infrared wavelengths) of the planet is still very faint: factor of ~1 million • Imaging of planets around Sun-like stars is currently not possible. Several ground-based and space- ...
NUMERICAL SIMULATIONS OF SOLAR AND STELLAR CONVECTION AND OSCILLATIONS By Dali Giorgobiani
... stochastically excite the resonant modes via Reynolds stresses and entropy fluctuations. Interaction between the convective motions and the waves modifies the mode frequencies, spectrum and amplitudes. We investigate turbulence and its interaction with oscillations by means of the realistic three-di ...
... stochastically excite the resonant modes via Reynolds stresses and entropy fluctuations. Interaction between the convective motions and the waves modifies the mode frequencies, spectrum and amplitudes. We investigate turbulence and its interaction with oscillations by means of the realistic three-di ...
$doc.title
... Figures 1 and 2. Since most of the variation in photoelectron flux intensity is seen above ...
... Figures 1 and 2. Since most of the variation in photoelectron flux intensity is seen above ...
![Detection of [Ne ii] Emission from Young Circumstellar Disks](http://s1.studyres.com/store/data/014394769_1-fdf9c6283148d488005c87b005dab353-300x300.png)
A new distance law of planets and satellites in the solar system
... observation. The similarity of (1) and (2) would have the constant a and b give a definite significance, but the physical mechanisms governing the formulas are quite different, so that the comparison of the formula (2) with the formula (1) would be meaningless. The proto-planet theory [15, 16], capt ...
... observation. The similarity of (1) and (2) would have the constant a and b give a definite significance, but the physical mechanisms governing the formulas are quite different, so that the comparison of the formula (2) with the formula (1) would be meaningless. The proto-planet theory [15, 16], capt ...
Models for GRBs and diverse transients
... thus reasonable to inquire as the outcome of jets of various powers released deep within the progenitor star. How long does it take jets of varying energy to break out? Is there a minimum power below which jets do not make it out at all, or takes such a long time that the star would surely have coll ...
... thus reasonable to inquire as the outcome of jets of various powers released deep within the progenitor star. How long does it take jets of varying energy to break out? Is there a minimum power below which jets do not make it out at all, or takes such a long time that the star would surely have coll ...
Basic Tools for Studies on the Formation and Disruption of Star
... no particular physical conditions are required. In this contribution we provide evidence that the LF of young clusters is not a −2 power law, but instead is curved, showing a systematic decrease of the (logarithmic) slope from roughly −1.8 at low luminosities to roughly −2.8 at high luminosities. Th ...
... no particular physical conditions are required. In this contribution we provide evidence that the LF of young clusters is not a −2 power law, but instead is curved, showing a systematic decrease of the (logarithmic) slope from roughly −1.8 at low luminosities to roughly −2.8 at high luminosities. Th ...
erice_091014 - Astronomy & Astrophysics Group
... e.g. 5 of the 9 SGBs in Berger et al (2007) had only X-ray positions, but these were measured to ~6 arcseconds. GW triggers from ET network would locate source to ~10 sq. deg. With only optical afterglows, that leaves ~107 galaxies! CHALLENGE Use 2nd generation NS-NS merger detections to better unde ...
... e.g. 5 of the 9 SGBs in Berger et al (2007) had only X-ray positions, but these were measured to ~6 arcseconds. GW triggers from ET network would locate source to ~10 sq. deg. With only optical afterglows, that leaves ~107 galaxies! CHALLENGE Use 2nd generation NS-NS merger detections to better unde ...
S-process in extremely metal-poor, low-mass stars
... the beginning of the thermally pulsating asymptotic giant branch (TP-AGB) phase. Similar to the occurrence of the PIE during the core He-flash, proton-rich material is dragged down into the He-burning zone during the development of a thermal runaway in the He-shell. After the ensuing dredge-up event ...
... the beginning of the thermally pulsating asymptotic giant branch (TP-AGB) phase. Similar to the occurrence of the PIE during the core He-flash, proton-rich material is dragged down into the He-burning zone during the development of a thermal runaway in the He-shell. After the ensuing dredge-up event ...
the Launching of Be-Star Disks
... feature of these RDOME models is to include the prograde radiative force that is expected in the region ahead of the bright spot. Since radiative driving is routinely capable of driving a stellar wind to speeds well in excess of orbital launch speeds, it seems in principal possible that the prograde ...
... feature of these RDOME models is to include the prograde radiative force that is expected in the region ahead of the bright spot. Since radiative driving is routinely capable of driving a stellar wind to speeds well in excess of orbital launch speeds, it seems in principal possible that the prograde ...
The Stromgren sphere around the highest-redshift QSOs
... are declining with time in a power-law form and the accretion process follows a self-similar evolutionary pattern as simple theoretical models predict. • Some other issues deserves of further investigation, such as the long-term evolution of accretion disks, the evolution of BBHs in QSOs/AGNs, coevo ...
... are declining with time in a power-law form and the accretion process follows a self-similar evolutionary pattern as simple theoretical models predict. • Some other issues deserves of further investigation, such as the long-term evolution of accretion disks, the evolution of BBHs in QSOs/AGNs, coevo ...
