Supernovae - Michigan State University
... If a stellar core grows beyond its Chandrasekhar mass limit, it will collapse. Typically this will result in a Supernova explosion at least the outer part of a star is blown off into space ...
... If a stellar core grows beyond its Chandrasekhar mass limit, it will collapse. Typically this will result in a Supernova explosion at least the outer part of a star is blown off into space ...
Distance Between Stars - cK-12
... than a few hundred light years away. For these more distant stars, astronomers must use more indirect methods of determining distance. Most of these methods involve determining how bright the star they are looking at really is. For example, if the star has properties similar to the Sun, then it shou ...
... than a few hundred light years away. For these more distant stars, astronomers must use more indirect methods of determining distance. Most of these methods involve determining how bright the star they are looking at really is. For example, if the star has properties similar to the Sun, then it shou ...
Stefan-Boltzmann`s law Wien`s law
... maximum wavelength corresponding to a black body spectrum of an extremely cold object of temperature of 2.7 K. Cosmological background radiation / Cosmic microwave background radiation (CMB) is microwave radiation - left over from the Big Bang that fills the universe roughly uniformly in all directi ...
... maximum wavelength corresponding to a black body spectrum of an extremely cold object of temperature of 2.7 K. Cosmological background radiation / Cosmic microwave background radiation (CMB) is microwave radiation - left over from the Big Bang that fills the universe roughly uniformly in all directi ...
chapter16StarBirth
... visible light • Observations of infrared light reveal stars on the other side of the cloud ...
... visible light • Observations of infrared light reveal stars on the other side of the cloud ...
PowerPoint
... • TMT/PFI can resolve outer side of planetary systems • Also, TMT may be able to detect a second Earth ...
... • TMT/PFI can resolve outer side of planetary systems • Also, TMT may be able to detect a second Earth ...
Part 3
... the light curve is not equal causes： 1 Asymmetry of the common envelope 2 Stellar dark spots model 3 Hot spots model problems： 1 We don’t know which mechanism is dominant 2 We don’t know the reason(s) which caused the O’connell effect type changes ...
... the light curve is not equal causes： 1 Asymmetry of the common envelope 2 Stellar dark spots model 3 Hot spots model problems： 1 We don’t know which mechanism is dominant 2 We don’t know the reason(s) which caused the O’connell effect type changes ...
Properties of Ellipticals and Spirals
... Magnitdes -7 to -22 Sizes 5 to 50 kpc Dust ~ 10% Warm gas Stars all population II in halo & Bulge; Population I otherwise • Colors B-V ~ mostly 0.9 Æ “red” • Metallicity varies though roughly solar to 3 times solar ...
... Magnitdes -7 to -22 Sizes 5 to 50 kpc Dust ~ 10% Warm gas Stars all population II in halo & Bulge; Population I otherwise • Colors B-V ~ mostly 0.9 Æ “red” • Metallicity varies though roughly solar to 3 times solar ...
ppt - Institute for Astronomy
... The solution is that FUor pairs are really quadruple systems which transformed from an unstable nonhierarchical configuration to an orderly hierarchical configuration. The quadruple then evolves slowly through viscous interactions until the components are so close that they erupt in FUor outbursts a ...
... The solution is that FUor pairs are really quadruple systems which transformed from an unstable nonhierarchical configuration to an orderly hierarchical configuration. The quadruple then evolves slowly through viscous interactions until the components are so close that they erupt in FUor outbursts a ...
15.1 Introduction
... Spectroscopically, WR stars are spectacular in appearance: their optical and UV spectra are dominated by strong, broad emission lines instead of the narrow absorption lines that are typical of ‘normal’ stars (Figure 15.3). The emission lines are so strong that they were first noticed as early as 186 ...
... Spectroscopically, WR stars are spectacular in appearance: their optical and UV spectra are dominated by strong, broad emission lines instead of the narrow absorption lines that are typical of ‘normal’ stars (Figure 15.3). The emission lines are so strong that they were first noticed as early as 186 ...
public_lector_10
... At the center of the bulge lies a supermassive black hole. Central BHs are common in galaxies: their mass is usually a small fraction of the bulge mass. ...
... At the center of the bulge lies a supermassive black hole. Central BHs are common in galaxies: their mass is usually a small fraction of the bulge mass. ...
astro2_lec1 - Astronomy & Astrophysics Group
... distances to dozens of nebulae. Even the nearest, in Andromeda, was millions of light ...
... distances to dozens of nebulae. Even the nearest, in Andromeda, was millions of light ...
A Hero`s Little Horse: Discovery of a Dissolving Star Cluster in
... limit of galaxy formation. The other new MW halo objects are star clusters with extremely low luminosities (−2.5 . MV . 0) and small half-light radii (< 10 pc). Globular clusters of such extreme nature are thought to be suffering stellar mass loss via dynamical processes such as tidal disruption or ...
... limit of galaxy formation. The other new MW halo objects are star clusters with extremely low luminosities (−2.5 . MV . 0) and small half-light radii (< 10 pc). Globular clusters of such extreme nature are thought to be suffering stellar mass loss via dynamical processes such as tidal disruption or ...
Introduction to Astronomy (high school)
... If one looks at this region with big telescopes and nearinfrared cameras one can see lots of stars. If one takes pictures every year it seems that some stars are moving very fast (up to 1500 kilometers per second). The fastest stars are in the very center - the position marked by the radio nucleus ...
... If one looks at this region with big telescopes and nearinfrared cameras one can see lots of stars. If one takes pictures every year it seems that some stars are moving very fast (up to 1500 kilometers per second). The fastest stars are in the very center - the position marked by the radio nucleus ...
neutron star - The University of Chicago
... capable to remove some of the outer, less gravitationally-bound layers. This wave-driven mass loss happens preferentially in either low mass (yet still massive) stars or lower metallicity more massive stars. Within a few months to a decade prior to CC up to ~1 Msun of material can be expelled. ...
... capable to remove some of the outer, less gravitationally-bound layers. This wave-driven mass loss happens preferentially in either low mass (yet still massive) stars or lower metallicity more massive stars. Within a few months to a decade prior to CC up to ~1 Msun of material can be expelled. ...
Stellar kinematics
Stellar kinematics is the study of the movement of stars without needing to understand how they acquired their motion. This differs from stellar dynamics, which takes into account gravitational effects. The motion of a star relative to the Sun can provide useful information about the origin and age of a star, as well as the structure and evolution of the surrounding part of the Milky Way.In astronomy, it is widely accepted that most stars are born within molecular clouds known as stellar nurseries. The stars formed within such a cloud compose open clusters containing dozens to thousands of members. These clusters dissociate over time. Stars that separate themselves from the cluster's core are designated as members of the cluster's stellar association. If the remnant later drifts through the Milky Way as a coherent assemblage, then it is termed a moving group.