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VLA OBSERVATIONS OF AMMONIA IN HIGH
VLA OBSERVATIONS OF AMMONIA IN HIGH

Formation Process of the Circumstellar Disk
Formation Process of the Circumstellar Disk

... We believe that stars are born with a circumstellar disk. The formation of the circumstellar disk is coupled with “the angular momentum problem” that is a serious problem in the star formation process, and the dynamics of disks may determine the mass accretion rate onto the protostar that determines ...
Gravitational-wave signal from binary neutron star merger
Gravitational-wave signal from binary neutron star merger

... simulation results with GW observation, or with analytical models, retaining the ability to distinguish the gravitational signal from different sources, for example, to be able to measure EOS-related effects, like tidal deformations in the final part of the pre-merger phase [90, 91]. The initial con ...
On the Rising of the Pleiades
On the Rising of the Pleiades

... sun, rising at sunset, culminating at midnight, and setting at sunrise (fig. 6). It is of interest—perhaps significance—that culmination in Hawai'i occurs at the zenith. But the Pleiades rising at opposition is a non-event; it cannot be seen. It can be predicted, though, and that requires a good cal ...
The occurrence of nitrogen-enhanced metal
The occurrence of nitrogen-enhanced metal

... 1/3, consistent with observations available to them, they find consistency with both the CEMP-s fraction (10–25%) and the CEMP-no/CEMP-s ratio for a top-heavy IMF, with a median mass of 10 M . Such proposed changes to the IMF would have profound consequences, since the IMF affects such diverse quan ...
First Results from the WISE Enhanced Resolution Galaxy Atlas
First Results from the WISE Enhanced Resolution Galaxy Atlas

Small glitches: the role of strange nuggets?
Small glitches: the role of strange nuggets?

The structure of steady detonation waves in Type Ia supernovae
The structure of steady detonation waves in Type Ia supernovae

MOLECULAR OUTFLOWS AND A MID
MOLECULAR OUTFLOWS AND A MID

... stellar objects in the filament with a combined stellar mass of 127  27 M. An additional 22 sources were identified as probable cluster members based on the presence of strong 24 m emission. The total star formation efficiency in the G34.4 cloud filament is estimated to be 7%, while the massive ...
White dwarfs, black holes and neutron stars in close binaries
White dwarfs, black holes and neutron stars in close binaries

The occurrence of nitrogen-enhanced metal
The occurrence of nitrogen-enhanced metal

... present a semi-analytical model for binary population synthesis, based on AGB models in which low-mass stars (0.8–1.5 M ) at [Fe/H] < −2.5 produce carbon and s-elements by dual shell flashes (see Sect. 5 for details). While this increases the parameter space for making CEMP-s stars considerably, it ...
An Optical Study of Young Stellar Clusters
An Optical Study of Young Stellar Clusters

ULTRA-COMPACT HII REGIONS AND MASSIVE STAR FORMATION
ULTRA-COMPACT HII REGIONS AND MASSIVE STAR FORMATION

... PUCHs are internally heated by the central massive protostar plus any associated lower-mass cluster members. They are likely to be surrounded by an equatorial accretion disk and a massive bipolar outflow along their spin axes. Their outflow masses, momenta, and kinetic energies are much larger than ...
The white dwarf luminosity function
The white dwarf luminosity function

... which are made of almost pure helium, only differing in effective temperature, which determines the corresponding spectral features, while DC white dwarfs are characterized by the absence of helium spectral lines at low temperatures. Although our basic understanding of the physical mechanisms that l ...
Massive Disruptions in the Cool Core of MACS J1931.8-2634 Steven Ehlert
Massive Disruptions in the Cool Core of MACS J1931.8-2634 Steven Ehlert

... Comparisons with Ophiuchus: Zoom ...
X-ray binaries in the Milky Way and other galaxies
X-ray binaries in the Milky Way and other galaxies

MUFASA: The assembly of the red sequence
MUFASA: The assembly of the red sequence

Post-starburst galaxies: more than just an interesting curiosity
Post-starburst galaxies: more than just an interesting curiosity

Photospheric processes and magnetic flux tubes
Photospheric processes and magnetic flux tubes

... The equations for a hydrostatic flux tube (cont.) Pizzo (1990) used a “body-fitted” nonorthogonal coordinate system to map the physical domain into a unit square computational domain. A multigrid elliptic solver is used at each iteration stage for solving Ampère’s equation. Fiedler & Cally (1991) ...
Full Text  - University of Toronto Astronomy
Full Text - University of Toronto Astronomy

A re-examination of galactic conformity and a comparison with semi
A re-examination of galactic conformity and a comparison with semi

... of the effect and how it changes as a function of the mass of the central galaxy. Conformity extends over a central galaxy stellar mass range spanning two orders of magnitude. The scale dependence and the precise nature of the effect depend on the mass of the central. In central galaxies with masses ...
Research Report for 2015/2016
Research Report for 2015/2016

... MS thesis described numerical work related to a new experimental design of a planetary magnetosphere. We obtained the first data with this platform last year, and have also initiated a new series of experiments in collaboration with C. Kuranz at the University of Michigan to study magnetized accreti ...
Modelling the observed properties of carbon-enhanced metal
Modelling the observed properties of carbon-enhanced metal

... system. In this work we generate synthetic populations of binary stars at metallicity Z = 0.0001 ([Fe/H] ≈ −2.3), with the aim of reproducing the observed fraction of CEMP stars in the halo. In addition, we aim to constrain our model of the wind masstransfer process, in particular the wind-accretion ...
Thesis (complete) - Research Explorer
Thesis (complete) - Research Explorer

... responsible for most of the energy produced. The production of energy via the CNOcycle depends much more strongly on temperature than the pp-chain does. Because of this, as the temperature in the core increases, for stars with progressively higher masses, the CNO-cycle gradually takes over as the ma ...
Pale Orange Dots: The Impact of Organic Haze on the Habitability
Pale Orange Dots: The Impact of Organic Haze on the Habitability

... Methane-rich terrestrial exoplanets with organic haze may occur frequently as methane (CH4 ) can be produced by several abiotic processes (Kasting 2005; Kelley et al. 2005; Etiope & Sherwood Lollar 2013; GuzmánMarmolejo et al. 2013), and CH4 -producing metabolisms (i.e., methanogenesis) are simple ...
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Standard solar model

The standard solar model (SSM) is a mathematical treatment of the Sun as a spherical ball of gas (in varying states of ionisation, with the hydrogen in the deep interior being a completely ionised plasma). This model, technically the spherically symmetric quasi-static model of a star, has stellar structure described by several differential equations derived from basic physical principles. The model is constrained by boundary conditions, namely the luminosity, radius, age and composition of the Sun, which are well determined. The age of the Sun cannot be measured directly; one way to estimate it is from the age of the oldest meteorites, and models of the evolution of the Solar System. The composition in the photosphere of the modern-day Sun, by mass, is 74.9% hydrogen and 23.8% helium. All heavier elements, called metals in astronomy, account for less than 2 percent of the mass. The SSM is used to test the validity of stellar evolution theory. In fact, the only way to determine the two free parameters of the stellar evolution model, the helium abundance and the mixing length parameter (used to model convection in the Sun), are to adjust the SSM to ""fit"" the observed Sun.
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