Chapter 13 Practice Questions
... A) mainly carbon and oxygen nuclei supported by electron degeneracy pressure in a volume about the size of the Sun. B) mostly hydrogen nuclei supported by normal gas pressure due to the very high gas temperature, in a volume about the size of the Earth. C) mainly carbon and oxygen nuclei supported b ...
... A) mainly carbon and oxygen nuclei supported by electron degeneracy pressure in a volume about the size of the Sun. B) mostly hydrogen nuclei supported by normal gas pressure due to the very high gas temperature, in a volume about the size of the Earth. C) mainly carbon and oxygen nuclei supported b ...
Document
... inward gravitational collapse is: a. Halted by degeneracy pressure in the core. b. Halted when the atoms are pushed up against one another and contraction stops. c. Finally balanced by outward thermal pressure from nuclear reactions. d. Finally balanced by radiation emitted in the photosphere. e. no ...
... inward gravitational collapse is: a. Halted by degeneracy pressure in the core. b. Halted when the atoms are pushed up against one another and contraction stops. c. Finally balanced by outward thermal pressure from nuclear reactions. d. Finally balanced by radiation emitted in the photosphere. e. no ...
Notes: Star Formation
... • The cloud of particles in a nebula begins to collapse because of gravity. – As the cloud collapses its temperature and density increase. – Temperature and density are the highest in the center of the cloud. – protostar- a dense area of gasses in a nebula that might become a star. ...
... • The cloud of particles in a nebula begins to collapse because of gravity. – As the cloud collapses its temperature and density increase. – Temperature and density are the highest in the center of the cloud. – protostar- a dense area of gasses in a nebula that might become a star. ...
The light curves for a nova look like the following.
... is electrically neutral and, therefore, not repulsed like the proton. there exist numerous free neutrons in the stars as the byproduct of many reactions. each neutron capture by heavy nuclei produces an isotope, some are stable, some are unstable. unstable isotopes will decay by emitting a positron ...
... is electrically neutral and, therefore, not repulsed like the proton. there exist numerous free neutrons in the stars as the byproduct of many reactions. each neutron capture by heavy nuclei produces an isotope, some are stable, some are unstable. unstable isotopes will decay by emitting a positron ...
21_LectureOutline
... • Stars greater than eight solar masses can have fusion in their cores going all the way up to iron, which is stable against further fusion. • The star continues to collapse after the iron core is found, implodes, and then explodes as a supernova. ...
... • Stars greater than eight solar masses can have fusion in their cores going all the way up to iron, which is stable against further fusion. • The star continues to collapse after the iron core is found, implodes, and then explodes as a supernova. ...
White Dwarf Stars
... During a star’s lifetime there are two forces fighting for control. The first is the inward force of gravity, trying to compress the star to as small a point as possible. Opposing gravity is the outward force of gas pressure provided by high temperatures inside the star. Although energy is lost by r ...
... During a star’s lifetime there are two forces fighting for control. The first is the inward force of gravity, trying to compress the star to as small a point as possible. Opposing gravity is the outward force of gas pressure provided by high temperatures inside the star. Although energy is lost by r ...
The Lives of Stars
... How do stars that can start fusion (M> 8% Msun) age? They spend most of their life cycle on the Main Sequence. Main Sequence stars fuse hydrogen into helium in their cores. Main Sequence stars are in hydrostatic equilibrium. ...
... How do stars that can start fusion (M> 8% Msun) age? They spend most of their life cycle on the Main Sequence. Main Sequence stars fuse hydrogen into helium in their cores. Main Sequence stars are in hydrostatic equilibrium. ...
The Life Cycles of Stars MEDIUM STARS MASSIVE STARS
... The Life Cycles of Stars A star's life cycle is determined by its mass. The larger the mass, the shorter the life cycle. A star's mass is determined by the amount of matter that is available in its nebula, the giant cloud of gas and dust in which it is born. Over time, gravity pulls the hydrogen gas ...
... The Life Cycles of Stars A star's life cycle is determined by its mass. The larger the mass, the shorter the life cycle. A star's mass is determined by the amount of matter that is available in its nebula, the giant cloud of gas and dust in which it is born. Over time, gravity pulls the hydrogen gas ...
Lecture 29: Ellipticals and Irregulars
... Methods of learning about what’s in galaxies: Images: use blue and red filters to measure colors and make H-R diagram from individual stars Integrated light/spectra Emission lines, particularly from neutral hydrogen and molecular gas. ...
... Methods of learning about what’s in galaxies: Images: use blue and red filters to measure colors and make H-R diagram from individual stars Integrated light/spectra Emission lines, particularly from neutral hydrogen and molecular gas. ...
SPY — The ESO Supernovae Type Ia Progenitor Survey
... dwarfs will, however, destroy themselves in a gigantic thermonuclear explosion. To do so, they have to be forced into a density and temperature regime, where carbon and oxygen burn explosively and disrupt the star. Above the Chandrasekhar mass (1.4 M) the electron degeneracy can no longer support w ...
... dwarfs will, however, destroy themselves in a gigantic thermonuclear explosion. To do so, they have to be forced into a density and temperature regime, where carbon and oxygen burn explosively and disrupt the star. Above the Chandrasekhar mass (1.4 M) the electron degeneracy can no longer support w ...
File
... A. Core-collapse of massive star B. Rebounding shock wave blows outer layers of star into space C. As bright as an entire galaxy! D. Signature: 1. Abundance of H2 2. Plateau in light curve ...
... A. Core-collapse of massive star B. Rebounding shock wave blows outer layers of star into space C. As bright as an entire galaxy! D. Signature: 1. Abundance of H2 2. Plateau in light curve ...
Chapter 2 Cosmic tombstones
... field A neutron star is formed, when a massive stellar core (> 1.4 M ) collapses, because it cannot support itself against its own weight. The continuing collapse is stopped by pressure of “neutron gas” produced from protons and electrons. Collapse leaves a newly formed neutron star very hot (milli ...
... field A neutron star is formed, when a massive stellar core (> 1.4 M ) collapses, because it cannot support itself against its own weight. The continuing collapse is stopped by pressure of “neutron gas” produced from protons and electrons. Collapse leaves a newly formed neutron star very hot (milli ...
kaekae14 dae dae15 lifecycleofastar
... cloud picks up stellar dust and other space junk the increasing gravity causes the cloud to collapse. As it collapses the cloud becomes smaller and hotter. After a few million years the low mass star begins to fuse helium into hydrogen. When this happens the collapse is ended because the fusion rais ...
... cloud picks up stellar dust and other space junk the increasing gravity causes the cloud to collapse. As it collapses the cloud becomes smaller and hotter. After a few million years the low mass star begins to fuse helium into hydrogen. When this happens the collapse is ended because the fusion rais ...
5Stars_Part_Two
... 3. Neutron stars are the size of towns. 4. Some Neutron stars spin a thousand times a second. 5. The pressure is so high in the core atomic nuclei cannot exist. 6. The outer envelope is about a mile thick - a crust of nuclei and electrons. 7. The core is a super-fluid. ...
... 3. Neutron stars are the size of towns. 4. Some Neutron stars spin a thousand times a second. 5. The pressure is so high in the core atomic nuclei cannot exist. 6. The outer envelope is about a mile thick - a crust of nuclei and electrons. 7. The core is a super-fluid. ...
Forging the elements
... At the end of the planetary nebula stage the star is left with an extremely hot, dense core (a million times denser than the earth). ...
... At the end of the planetary nebula stage the star is left with an extremely hot, dense core (a million times denser than the earth). ...
astr study guide ex 3 s`16
... 38. Where are elements heavier than iron can only be created ? 39. When the mass of a star's core becomes greater than 1.4 times the mass of the Sun, degenerate electrons can no longer keep it as a white dwarf. Instead, what does it become? 40. To predict whether a star will ultimately become a blac ...
... 38. Where are elements heavier than iron can only be created ? 39. When the mass of a star's core becomes greater than 1.4 times the mass of the Sun, degenerate electrons can no longer keep it as a white dwarf. Instead, what does it become? 40. To predict whether a star will ultimately become a blac ...
Ch. 21
... A high-mass star can continue to fuse elements in its core right up to iron (after which the fusion reaction is energetically unfavored). As heavier elements are fused, the reactions go faster and the stage is over more quickly. A 20-solar-mass star will burn carbon for ...
... A high-mass star can continue to fuse elements in its core right up to iron (after which the fusion reaction is energetically unfavored). As heavier elements are fused, the reactions go faster and the stage is over more quickly. A 20-solar-mass star will burn carbon for ...
The Main Sequence
... • From Red Giant cores to White Dwarfs to Neutron Stars, density has been increasing. • As density increases, the force of gravity on the surface increases. • The greater the force, the higher the escape velocity: – How fast you need to go in order to escape the surface. • How dense can something ge ...
... • From Red Giant cores to White Dwarfs to Neutron Stars, density has been increasing. • As density increases, the force of gravity on the surface increases. • The greater the force, the higher the escape velocity: – How fast you need to go in order to escape the surface. • How dense can something ge ...
HD 91669b: A New Brown Dwarf Candidate from the McDonald
... 90◦ , is only 0.9 mas peak-to-peak. It is clear that this would be too small to be significantly detectable by Hipparcos. Thus, while we cannot derive a tight constraint on the companion mass, the Hipparcos data are at least not inconsistent with a companion mass in the brown dwarf regime. The orbit ...
... 90◦ , is only 0.9 mas peak-to-peak. It is clear that this would be too small to be significantly detectable by Hipparcos. Thus, while we cannot derive a tight constraint on the companion mass, the Hipparcos data are at least not inconsistent with a companion mass in the brown dwarf regime. The orbit ...
An automated 2 epoch Proper Motion search of UKIDSS and VISTA
... finding very cold brown dwarfs. Objects too faint for normal multiband colour selection, or those with unusual colours (e.g. recent WISE 300 K object). brown dwarf companions to stars. These are benchmark objects with known age, metallicity and Hipparcos distance that can be used to test model atmos ...
... finding very cold brown dwarfs. Objects too faint for normal multiband colour selection, or those with unusual colours (e.g. recent WISE 300 K object). brown dwarf companions to stars. These are benchmark objects with known age, metallicity and Hipparcos distance that can be used to test model atmos ...
Sample Final
... 39. Of the following reaction chains, which is not part of the proton-proton chain? a) ...
... 39. Of the following reaction chains, which is not part of the proton-proton chain? a) ...
Stellar Explosions
... A high-mass star can continue to fuse elements in its core right up to iron (after which the fusion reaction is energetically unfavored). As heavier elements are fused, the reactions go faster and the stage is over more quickly. A 20-solar-mass star will burn carbon for ...
... A high-mass star can continue to fuse elements in its core right up to iron (after which the fusion reaction is energetically unfavored). As heavier elements are fused, the reactions go faster and the stage is over more quickly. A 20-solar-mass star will burn carbon for ...