1. The figure below represents the planet Jupiter. The centre of the
... The equation of state of an ideal gas is pV = nRT. Data about gases are often given in terms of density rather than volume V. Show that the equation of state for a gas can be written as p = RT/M where M is the mass of one mole of gas. ...
... The equation of state of an ideal gas is pV = nRT. Data about gases are often given in terms of density rather than volume V. Show that the equation of state for a gas can be written as p = RT/M where M is the mass of one mole of gas. ...
The half-light radius distribution of LBGs and their
... • There exists an correlation between r_ff and SFR --- imply that the star forming regions are disk-like; • Star formation timescale is about 0.3Gyr • Duty cycle effect is important for LBGs ---- there should exist non-LBG population with massive stellar mass at z~ 3 which can be detected by Spitzer ...
... • There exists an correlation between r_ff and SFR --- imply that the star forming regions are disk-like; • Star formation timescale is about 0.3Gyr • Duty cycle effect is important for LBGs ---- there should exist non-LBG population with massive stellar mass at z~ 3 which can be detected by Spitzer ...
Accretion
... Since viscosity drives accretion a ~ dM/dt - one determines a by measuring the accretion rate using observations of accretion disk luminosity/spectrum. It turns out that typically a ~ 10-1– 1 for accretion disks around compact objects (e.g. black holes), 10-3 – 10-2 for protostellar disks. ...
... Since viscosity drives accretion a ~ dM/dt - one determines a by measuring the accretion rate using observations of accretion disk luminosity/spectrum. It turns out that typically a ~ 10-1– 1 for accretion disks around compact objects (e.g. black holes), 10-3 – 10-2 for protostellar disks. ...
FP11: DRAKE et al. - Astronomical Institute WWW Homepage
... line profile, brightness, and magnetic field as a function of the rotating phase, which can be explained in terms of an oblique magnetic rotator model. We estimated the effective temperature, surface gravity, mass, luminosity, and radius of this star, as well as the inclination angle of the rotation ...
... line profile, brightness, and magnetic field as a function of the rotating phase, which can be explained in terms of an oblique magnetic rotator model. We estimated the effective temperature, surface gravity, mass, luminosity, and radius of this star, as well as the inclination angle of the rotation ...
Numerical simulations of aligned neutron star magnetospheres
... magnetosphere consists of a dome above the polar cap containing plasma of one charge and an equatorial belt containing plasma of the other sign: E ´ B 0 inside both of these. These are separated by a vacuum gap in which E ´ B ± 0 r 0 instead). We show that the charge distribution used in the `s ...
... magnetosphere consists of a dome above the polar cap containing plasma of one charge and an equatorial belt containing plasma of the other sign: E ´ B 0 inside both of these. These are separated by a vacuum gap in which E ´ B ± 0 r 0 instead). We show that the charge distribution used in the `s ...
The Life of a Star
... where d is the distance in parsec (3:08 1018 cm); M correponds to the brightness at 10 pc. m M is also called distance modulus; 0:2(m M ) + 1 = log d. Magnitudes measured in a wavelength band are denoted by their indices, e.g. MV or mB . If the total or bolometric luminosity or brightness is meant ...
... where d is the distance in parsec (3:08 1018 cm); M correponds to the brightness at 10 pc. m M is also called distance modulus; 0:2(m M ) + 1 = log d. Magnitudes measured in a wavelength band are denoted by their indices, e.g. MV or mB . If the total or bolometric luminosity or brightness is meant ...
W. M. White Geochemistry Chapter 10: Cosmochemistry
... we learn about the evolution of the Earth by examining old rocks, we can learn about the evolution of the cosmos by looking at old stars. The old stars of Population II are considerably poorer in heavy elements than are young stars. In particular, Population II stars have a Fe/H ratio typically a fa ...
... we learn about the evolution of the Earth by examining old rocks, we can learn about the evolution of the cosmos by looking at old stars. The old stars of Population II are considerably poorer in heavy elements than are young stars. In particular, Population II stars have a Fe/H ratio typically a fa ...
Simulations of Collisionless Perpendicular Shocks in Partially
... another scale length of the order of 103 c/ωpp that corresponds to the ionization length scale. In the upstream and downstream regions, the plasma flow is gradually decelerated by the pressure of pickup ions produced in upstream and downstream regions. In this Letter, charge exchange and collisional ...
... another scale length of the order of 103 c/ωpp that corresponds to the ionization length scale. In the upstream and downstream regions, the plasma flow is gradually decelerated by the pressure of pickup ions produced in upstream and downstream regions. In this Letter, charge exchange and collisional ...
On the anomalous mass defect of strange stars in the Field
... general overview shows us that anomalous mass defects can (in principle) be obtained for arbitrary values of the model parameters. If G2 is low, V1 must be increased in order to yield anomalous mass defect; if V1 is low, G2 must grow in order to produce the same effect. As it was stated above, new r ...
... general overview shows us that anomalous mass defects can (in principle) be obtained for arbitrary values of the model parameters. If G2 is low, V1 must be increased in order to yield anomalous mass defect; if V1 is low, G2 must grow in order to produce the same effect. As it was stated above, new r ...
Extreme abundance ratios in the polluted atmosphere of the cool
... that at least 27 per cent of their white dwarf sample, which includes the Gänsicke et al. (2012) sample, would be currently accreting, while in 29 per cent of these objects, usually among the warmest in their sample, the effect of radiative levitation dominates the abundance pattern. The inclusion ...
... that at least 27 per cent of their white dwarf sample, which includes the Gänsicke et al. (2012) sample, would be currently accreting, while in 29 per cent of these objects, usually among the warmest in their sample, the effect of radiative levitation dominates the abundance pattern. The inclusion ...
Reconciling observations and modelling of thermonuclear bursts
... “precision” nuclear astrophysics from thermonuclear bursts Meaning, we want to reduce the astrophysical uncertainties for observations of bursts, to the point where we are sensitive to the nuclear ...
... “precision” nuclear astrophysics from thermonuclear bursts Meaning, we want to reduce the astrophysical uncertainties for observations of bursts, to the point where we are sensitive to the nuclear ...
A timeline of the universe
... first star was poised to form. To make a star, matter must collapse into the bottom of a gravitational well. The more gas that falls into the well, the higher the density. Eventually, nuclear fusion occurs, and the star turns on. Astronomers understand how stars form in the current cosmos and know e ...
... first star was poised to form. To make a star, matter must collapse into the bottom of a gravitational well. The more gas that falls into the well, the higher the density. Eventually, nuclear fusion occurs, and the star turns on. Astronomers understand how stars form in the current cosmos and know e ...
PPT - GSI
... 1.) Droplet model (DM) [Myers 1977], which is a basis of often used results of the Howard-Möller fission-barrier calculations [Howard&Möller 1980] 2.) Finite-range liquid drop model (FRLDM) [Sierk 1986, Möller et al 1995] 3.) Thomas-Fermi model (TF) [Myers&Swiatecki 1996, 1999] 4.) Extended Thomas-F ...
... 1.) Droplet model (DM) [Myers 1977], which is a basis of often used results of the Howard-Möller fission-barrier calculations [Howard&Möller 1980] 2.) Finite-range liquid drop model (FRLDM) [Sierk 1986, Möller et al 1995] 3.) Thomas-Fermi model (TF) [Myers&Swiatecki 1996, 1999] 4.) Extended Thomas-F ...
Who’s Afraid of a Stellar Superflare? Rachel Osten GSFC
... superflaring in normal stars -- Schaefer et al. (2000) normal solar-like stars undergoing flaring events with energy releases 1033-1038 ergs, occurring roughly once every 100 years or so ...
... superflaring in normal stars -- Schaefer et al. (2000) normal solar-like stars undergoing flaring events with energy releases 1033-1038 ergs, occurring roughly once every 100 years or so ...
Formation of millisecond pulsars with CO white dwarf companions–I
... value may not be universal and could, for example, depend on the stellar mass ratio in a given binary. During the very short spiral-in and ejection phase of a common envelope evolution (∼103 yr) it is a good approximation to assume that the neutron star does not accrete any significant amount of mat ...
... value may not be universal and could, for example, depend on the stellar mass ratio in a given binary. During the very short spiral-in and ejection phase of a common envelope evolution (∼103 yr) it is a good approximation to assume that the neutron star does not accrete any significant amount of mat ...
Sample pages 1 PDF
... increasing force of electrostatic repulsion of their positive charges, which is described by Coulomb and defined as Coulomb force and results in some barrier that is known as Coulomb barrier. In the fusion of light elements to form heavier ones, the nuclei (which carry positive electrical charge) mu ...
... increasing force of electrostatic repulsion of their positive charges, which is described by Coulomb and defined as Coulomb force and results in some barrier that is known as Coulomb barrier. In the fusion of light elements to form heavier ones, the nuclei (which carry positive electrical charge) mu ...
HWWS 2010 - Monash University
... But what about black holes? • Black holes are more compact but have no surface so energy may be lost through the event horizon • To eke out a final few ergs the accreted material on neutron stars may undergo stable and/or unstable thermonuclear burning ...
... But what about black holes? • Black holes are more compact but have no surface so energy may be lost through the event horizon • To eke out a final few ergs the accreted material on neutron stars may undergo stable and/or unstable thermonuclear burning ...
Self-Regulation of Star Formation in Low Metallicity Clouds
... stars in the cold clouds, and the star formation throughout the clouds. However, the mass of the first generation stars are estimated through detailed investigation to be fairly large (Nakamura & Umemura 1999, Omukai & Nishi 1998). Thus, the third step is disturbed by the feedback from the massive s ...
... stars in the cold clouds, and the star formation throughout the clouds. However, the mass of the first generation stars are estimated through detailed investigation to be fairly large (Nakamura & Umemura 1999, Omukai & Nishi 1998). Thus, the third step is disturbed by the feedback from the massive s ...
Introduc on to the Fundamental Astrophysics Course
... Introduc)on to the Fundamental Astrophysics Course -‐ 2013 ...
... Introduc)on to the Fundamental Astrophysics Course -‐ 2013 ...
Chapter 5 Theory of Stellar Evolution
... How are we to reconcile these impediments to gravitational contraction with the fact that stars exits? One can use the rotational and magnetic energies against one another. A moderate magnetic field of a spinning object will cause a great deal of angular momentum per unit mass to be lost by a star t ...
... How are we to reconcile these impediments to gravitational contraction with the fact that stars exits? One can use the rotational and magnetic energies against one another. A moderate magnetic field of a spinning object will cause a great deal of angular momentum per unit mass to be lost by a star 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.