Unresolved Stellar Populations
... this does not help much for a young SSP (for which the color of AGB and/or RGB also depends on the age). There are also other potential uncertainties: • For an SSP with mass < 106 M , the color may be subject to large statistical fluctuations caused by the small number of upper RGB and AGB stars. • ...
... this does not help much for a young SSP (for which the color of AGB and/or RGB also depends on the age). There are also other potential uncertainties: • For an SSP with mass < 106 M , the color may be subject to large statistical fluctuations caused by the small number of upper RGB and AGB stars. • ...
Goal: To understand the HR diagram
... • Meanwhile the V value does not change much. • Therefore B-V increases as temperatures drop. • In fact, a B-V value is the indicator of a specific temperature of star! ...
... • Meanwhile the V value does not change much. • Therefore B-V increases as temperatures drop. • In fact, a B-V value is the indicator of a specific temperature of star! ...
Week 9
... Thought Question: When I pass a jug of clear blue liquid in front of the light bulb, what will happen? A. The jug will make the violet, blue, and green light more intense. B. The jug will make the yellow, orange, and red light more intense. C. The jug will remove most of the violet, blue, and green ...
... Thought Question: When I pass a jug of clear blue liquid in front of the light bulb, what will happen? A. The jug will make the violet, blue, and green light more intense. B. The jug will make the yellow, orange, and red light more intense. C. The jug will remove most of the violet, blue, and green ...
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... The effect of dark energy on the expansion of the Universe is that the expansion is _____ ...
... The effect of dark energy on the expansion of the Universe is that the expansion is _____ ...
Dark Matter Dark Energy The History of the Universe More of the
... The effect of dark energy on the expansion of the Universe is that the expansion is _____ ...
... The effect of dark energy on the expansion of the Universe is that the expansion is _____ ...
The Sun's Crowded Delivery Room July 6, 2007
... The 60Fe cannot have come from a source too far from the infant Sun. If too far away it would decay before arriving or be so diluted that we could not measure it. The exploding star had to be in the Sun's general vicinity. It was a cluster mate of the Sun. One type of massive star is called a Wolf-R ...
... The 60Fe cannot have come from a source too far from the infant Sun. If too far away it would decay before arriving or be so diluted that we could not measure it. The exploding star had to be in the Sun's general vicinity. It was a cluster mate of the Sun. One type of massive star is called a Wolf-R ...
poster
... compare evolutionary trends with other young star forming clusters. We present results of our multiwavelength study of IRAS 20050+2720 which includes observations by Chandra, Spitzer, and 2MASS and UBVRI photometry. In total, about 300 YSOs in ...
... compare evolutionary trends with other young star forming clusters. We present results of our multiwavelength study of IRAS 20050+2720 which includes observations by Chandra, Spitzer, and 2MASS and UBVRI photometry. In total, about 300 YSOs in ...
DETAILED STELLAR POPULATION ANALYSIS OF GALAXY
... were chosen based on their X-ray luminosities. The sample is limited to clusters with X-ray luminosities larger than LX = 2 × 1044 ergs per second and is intended to be representative of rich galaxy clusters. The galaxies for which spectra were obtained can be several times less luminous than the Mi ...
... were chosen based on their X-ray luminosities. The sample is limited to clusters with X-ray luminosities larger than LX = 2 × 1044 ergs per second and is intended to be representative of rich galaxy clusters. The galaxies for which spectra were obtained can be several times less luminous than the Mi ...
NGC 3801 caught in the act: A post-merger starforming early
... more similar to the hysteresis loop. The radio lobes, also in the shape of S, is seen confined within this hysteresis loop structure (HLS), with similar clockwise bending (See Fig.1; Heckman et al. 1986). Surrounding these radio lobes, shock shells have been discovered with the Chandra X-ray observa ...
... more similar to the hysteresis loop. The radio lobes, also in the shape of S, is seen confined within this hysteresis loop structure (HLS), with similar clockwise bending (See Fig.1; Heckman et al. 1986). Surrounding these radio lobes, shock shells have been discovered with the Chandra X-ray observa ...
Images
... the phase space), and whose numbers are conserved (no creation or destruction of particles). Since these are also conditions for stars in a galaxy, then the DF for stars in a galaxy must be such that it is a solution to the CBE. c) Consider following a star as it moves through the 6-D phase space. W ...
... the phase space), and whose numbers are conserved (no creation or destruction of particles). Since these are also conditions for stars in a galaxy, then the DF for stars in a galaxy must be such that it is a solution to the CBE. c) Consider following a star as it moves through the 6-D phase space. W ...
black holes activity
... -The gas particles in the core and radiation zone ____________ with each other constantly but by the time it get to 200,000 km out it is turned into energy and through convection transferred towards the surface C.What is Granulation? -Looking at the surface of the Sun it looks highly _______________ ...
... -The gas particles in the core and radiation zone ____________ with each other constantly but by the time it get to 200,000 km out it is turned into energy and through convection transferred towards the surface C.What is Granulation? -Looking at the surface of the Sun it looks highly _______________ ...
question - UW Canvas
... 23. How is it that the core of a massive star is able to fuse heavier and heavier elements without any of these stages resulting in degeneracy or any flashes like the helium flash that occurs in solar-type stars? a. The cores of massive stars are so hot, have such high densities and pressures, that ...
... 23. How is it that the core of a massive star is able to fuse heavier and heavier elements without any of these stages resulting in degeneracy or any flashes like the helium flash that occurs in solar-type stars? a. The cores of massive stars are so hot, have such high densities and pressures, that ...
Dark Matter Capture in the first stars
... the core may fill in with DM again s.t. annihilation heating continues for a longer time Are there still some dark stars around today? ...
... the core may fill in with DM again s.t. annihilation heating continues for a longer time Are there still some dark stars around today? ...
Chapter 7 Stellar models and stellar stability
... shall prove shortly) the same relative density distribution. All models have to obey the stellar structure equations, so that the transition for one homologous model to another has consequences for all other variables. We start by analysing the first two structure equations. • The first stellar stru ...
... shall prove shortly) the same relative density distribution. All models have to obey the stellar structure equations, so that the transition for one homologous model to another has consequences for all other variables. We start by analysing the first two structure equations. • The first stellar stru ...
1 The Gravitational Field Gravitational Potential Energy Grav
... hole and a normal star, the material from the normal star can be pulled into the black hole This material forms an accretion disk around the black hole Friction among the particles in the disk transforms mechanical energy into internal energy ...
... hole and a normal star, the material from the normal star can be pulled into the black hole This material forms an accretion disk around the black hole Friction among the particles in the disk transforms mechanical energy into internal energy ...
Untitled - Notion Press
... solar mass end with a ‘supernova.’ The stars of these masses leave superheated plasma during supernova. The energy of this star is released in the form of light and neutrino. Neutrino is also a type of sub-atomic particle. The stuff remaining after supernova is a compact ball of entirely neutrons. I ...
... solar mass end with a ‘supernova.’ The stars of these masses leave superheated plasma during supernova. The energy of this star is released in the form of light and neutrino. Neutrino is also a type of sub-atomic particle. The stuff remaining after supernova is a compact ball of entirely neutrons. I ...
Properties of Stars - Indiana State University
... • The Stefan-Boltzmann law is a key to understanding the H-R diagram – For stars of a given temperature, the larger the radius, the larger the luminosity – Therefore, as one moves up the H-R diagram, a star’s radius must become bigger – On the other hand, for a given luminosity, the larger the radiu ...
... • The Stefan-Boltzmann law is a key to understanding the H-R diagram – For stars of a given temperature, the larger the radius, the larger the luminosity – Therefore, as one moves up the H-R diagram, a star’s radius must become bigger – On the other hand, for a given luminosity, the larger the radiu ...
Next Generation VLA Science White Paper
... to study the detailed astrophysics of star formation both within the Milky Way and nearby galaxies. With an unprecedented combination of high angular resolution and both line and continuum sensitivity, this revolutionary facility will: (1) provide new insight on the fundamental physics behind radio ...
... to study the detailed astrophysics of star formation both within the Milky Way and nearby galaxies. With an unprecedented combination of high angular resolution and both line and continuum sensitivity, this revolutionary facility will: (1) provide new insight on the fundamental physics behind radio ...
PowerPoint Presentation - 21. Galaxy Evolution
... • With such a fast rate of star formation, the galaxy will use up its gas.. • in only a few 100 million years • starburst phase is temporary in light of fact that galaxy is billions of years old © 2004 Pearson Education Inc., publishing as Addison-Wesley ...
... • With such a fast rate of star formation, the galaxy will use up its gas.. • in only a few 100 million years • starburst phase is temporary in light of fact that galaxy is billions of years old © 2004 Pearson Education Inc., publishing as Addison-Wesley ...
AST 1010 Quiz questions
... 1. Construct a correctly labeled H-R diagram. Include the following regions: the main sequence, giants, supergiants, and white dwarfs. Be sure to label your axes. Draw on the same diagram a line that traces the evolutionary path of a star like our Sun from the time the giant molecular cloud begins t ...
... 1. Construct a correctly labeled H-R diagram. Include the following regions: the main sequence, giants, supergiants, and white dwarfs. Be sure to label your axes. Draw on the same diagram a line that traces the evolutionary path of a star like our Sun from the time the giant molecular cloud begins t ...
Quasars - Ann Arbor Earth Science
... radio galaxy - a galaxy showing unusually strong radio emission, too intense to be produced by the normal processes of starbirth and stardeath. This may come only from the nucleus, or from a pair of more or less symmetric lobes stretching as far as a million light-years. Many show emission from je ...
... radio galaxy - a galaxy showing unusually strong radio emission, too intense to be produced by the normal processes of starbirth and stardeath. This may come only from the nucleus, or from a pair of more or less symmetric lobes stretching as far as a million light-years. Many show emission from je ...
Galaxy Structure
... In the last few years, independent evidence points to the existence of a bar in the inner Galaxy. This evidence results from NIR photometry (Blitz and Spergel 1991; Weiland et al 1994; Dwek et al 1995), from IRAS source counts (Nakada et al 1991; Whitelock and Catchpole 1992; Nikolaev and Weinberg 1 ...
... In the last few years, independent evidence points to the existence of a bar in the inner Galaxy. This evidence results from NIR photometry (Blitz and Spergel 1991; Weiland et al 1994; Dwek et al 1995), from IRAS source counts (Nakada et al 1991; Whitelock and Catchpole 1992; Nikolaev and Weinberg 1 ...
Star formation
Star formation is the process by which dense regions within molecular clouds in interstellar space, sometimes referred to as ""stellar nurseries"" or ""star-forming regions"", collapse to form stars. As a branch of astronomy, star formation includes the study of the interstellar medium (ISM) and giant molecular clouds (GMC) as precursors to the star formation process, and the study of protostars and young stellar objects as its immediate products. It is closely related to planet formation, another branch of astronomy. Star formation theory, as well as accounting for the formation of a single star, must also account for the statistics of binary stars and the initial mass function.In June 2015, astronomers reported evidence for Population III stars in the Cosmos Redshift 7 galaxy at z = 6.60. Such stars are likely to have existed in the very early universe (i.e., at high redshift), and may have started the production of chemical elements heavier than hydrogen that are needed for the later formation of planets and life as we know it.