Gravitational Radiation from Rotating White Dwarfs and
... Gravitational waves from isolated sources like single neutron stars or white dwarfs aren’t as much intense as comparably very rare events in massive double systems, but the quantity of single stars and comparably small distances to Earth make these sources interesting from viewpoint of gravitational ...
... Gravitational waves from isolated sources like single neutron stars or white dwarfs aren’t as much intense as comparably very rare events in massive double systems, but the quantity of single stars and comparably small distances to Earth make these sources interesting from viewpoint of gravitational ...
The habitability and detection of Earth
... Earth (Agol 2011). Raven (2007) concluded that photosynthesis can occur on exoplanets in the habitable zone of M dwarfs. The photosynthetic relevant flux intercepted by a planet in the CHZ of a 4000 K white dwarf is larger than that intercepted by the same planet in the habitable zone of a typical M ...
... Earth (Agol 2011). Raven (2007) concluded that photosynthesis can occur on exoplanets in the habitable zone of M dwarfs. The photosynthetic relevant flux intercepted by a planet in the CHZ of a 4000 K white dwarf is larger than that intercepted by the same planet in the habitable zone of a typical M ...
PowerPoint Presentation - 18. The Bizarre Stellar Graveyard
... masses collapses beyond electron degeneracy, to a much denser object, where neutron degeneracy holds the object up against gravity - neutron star, seen from some angles looks like a pulsing object (pulsar) • Cores > 3 solar mass collapse beyond this, to a black hole we have no physical model for wha ...
... masses collapses beyond electron degeneracy, to a much denser object, where neutron degeneracy holds the object up against gravity - neutron star, seen from some angles looks like a pulsing object (pulsar) • Cores > 3 solar mass collapse beyond this, to a black hole we have no physical model for wha ...
Manuscript - Kapteyn Astronomical Institute
... In the case of gas-rich systems –which are a majority at the low mass end, encounters with dark satellites will be less efficient at changing the structure of the host dwarf galaxy, because much of the orbital energy will be absorbed by the gas, leading to less vertical heating. However, we may expe ...
... In the case of gas-rich systems –which are a majority at the low mass end, encounters with dark satellites will be less efficient at changing the structure of the host dwarf galaxy, because much of the orbital energy will be absorbed by the gas, leading to less vertical heating. However, we may expe ...
Document
... Remember there was no dependence on me, c, or R in the extreme relativistic limit. ...
... Remember there was no dependence on me, c, or R in the extreme relativistic limit. ...
Dust [12.1]
... • Often, wavelength resolution and/or signal:noise too low to measure details of line profile. • Can still measure fraction of continuum light that is absorbed • then convert to column density of absorbing atoms. ...
... • Often, wavelength resolution and/or signal:noise too low to measure details of line profile. • Can still measure fraction of continuum light that is absorbed • then convert to column density of absorbing atoms. ...
Is the initial mass function universal?
... Clump mass spectrum in low-mass and highmass regions covers the whole mass spectrum. is the IMF a product of the cloud power spectrum (Motte et al. 1998, Beuther ...
... Clump mass spectrum in low-mass and highmass regions covers the whole mass spectrum. is the IMF a product of the cloud power spectrum (Motte et al. 1998, Beuther ...
White dwarfmain sequence binaries identified within SDSS DR7 and
... secondary stars and the metallicities of the secondaries. Meanwhile, we determine the cooling age via interpolation through evolutionary models for the effective temperature and surface gravity of each DA white dwarf. Distributions of these stellar parameters have been used to study both the general ...
... secondary stars and the metallicities of the secondaries. Meanwhile, we determine the cooling age via interpolation through evolutionary models for the effective temperature and surface gravity of each DA white dwarf. Distributions of these stellar parameters have been used to study both the general ...
HR Diagrams
... Do you think that taller students tend to weigh more or less than shorter students? You could examine this by plotting the students in your class on a graph, with height on one axis and weight on the other. Each student would be plotted as a point on the graph. What do you think that graph would loo ...
... Do you think that taller students tend to weigh more or less than shorter students? You could examine this by plotting the students in your class on a graph, with height on one axis and weight on the other. Each student would be plotted as a point on the graph. What do you think that graph would loo ...
Components of the Milky Way
... M < 13 MJupiter ~ 10-2 Msun: no significant nuclear fusion at all `Planetary mass objects’ 13 MJ < M < 0.08 Msun: deuterium fusion but no fusion of ordinary hydrogen - brown dwarfs M ~ 100 Msun: very rough upper limit set by radiation pressure On main sequence, mass largely sets the luminosity, radi ...
... M < 13 MJupiter ~ 10-2 Msun: no significant nuclear fusion at all `Planetary mass objects’ 13 MJ < M < 0.08 Msun: deuterium fusion but no fusion of ordinary hydrogen - brown dwarfs M ~ 100 Msun: very rough upper limit set by radiation pressure On main sequence, mass largely sets the luminosity, radi ...
Stability of hot neutron stars
... It is likely that matter in a neutron star crust is compressed by accreting matter and/or by the slowingdown of its rotation after the freezing of thermonuclear equilibrium. The change of nuclear compositions, which takes place during the compression, has been investigated. If the initial species of ...
... It is likely that matter in a neutron star crust is compressed by accreting matter and/or by the slowingdown of its rotation after the freezing of thermonuclear equilibrium. The change of nuclear compositions, which takes place during the compression, has been investigated. If the initial species of ...
Structure of Neutron Stars - Relativistic Astrophysics Department
... Minimum-mass M ~ 0.1 M Sun neutron star R ~ 250 km ...
... Minimum-mass M ~ 0.1 M Sun neutron star R ~ 250 km ...
Name: Period: _____ Stars Interactives and Activities
... 4. What are the two ways the x-axis can be labeled? ...
... 4. What are the two ways the x-axis can be labeled? ...
Astronomy 112: The Physics of Stars Class 9 Notes: Polytropes With
... n = 1.5 to n = 3. Thus we expect a nearly universal relation among the central pressure, central density and mass of stars. C. The Chandrasekhar Mass and Relativistic Gasses Consider what this analysis of polytropes implies for stars where the pressure is dominated by electron degeneracy pressure. W ...
... n = 1.5 to n = 3. Thus we expect a nearly universal relation among the central pressure, central density and mass of stars. C. The Chandrasekhar Mass and Relativistic Gasses Consider what this analysis of polytropes implies for stars where the pressure is dominated by electron degeneracy pressure. W ...
Stellar Evolution Game (PDF: 112k)
... Connection to Space Odyssey During your visit to Space Odyssey have students explore the Life of a Star interactive. Students will be able to apply their knowledge from this activity to the concepts learned in the interactive. ...
... Connection to Space Odyssey During your visit to Space Odyssey have students explore the Life of a Star interactive. Students will be able to apply their knowledge from this activity to the concepts learned in the interactive. ...
ASTR 1020 General Astronomy: Stars and Galaxies REVIEW
... Regular stars need thermal pressure to balance gravity, and they need nuclear reactions to maintain the pressure, so the die when they run out of fuel. Not so White Dwarfs. They are as stable as a rock. Literally. A quadrillion years in the future all the stars will be gone, but the White Dwarfs wil ...
... Regular stars need thermal pressure to balance gravity, and they need nuclear reactions to maintain the pressure, so the die when they run out of fuel. Not so White Dwarfs. They are as stable as a rock. Literally. A quadrillion years in the future all the stars will be gone, but the White Dwarfs wil ...
White dwarf dynamical interactions and fast optical transients
... be very fast, and a common result is that the disruption takes place in a few orbital periods for the case of white dwarf mergers, and on short timescales for white dwarf collisions in which the low-mass member of the pair is captured in a highly eccentric orbit, typically in a few orbits as well. I ...
... be very fast, and a common result is that the disruption takes place in a few orbital periods for the case of white dwarf mergers, and on short timescales for white dwarf collisions in which the low-mass member of the pair is captured in a highly eccentric orbit, typically in a few orbits as well. I ...
Neutrino Masses, Dark Matter and the Mysterious Early Quasars
... within a radius rC from the centre is ...
... within a radius rC from the centre is ...
Chapter 25.2 - Planet Earth
... Degenerate matter uses electrical repulsion instead of molecular motion to support itself from total collapse. Although atomic particles in degenerate matter are much closer together than in normal Earth matter, they still are not packed as tightly as possible. Stars made of matter that has an even ...
... Degenerate matter uses electrical repulsion instead of molecular motion to support itself from total collapse. Although atomic particles in degenerate matter are much closer together than in normal Earth matter, they still are not packed as tightly as possible. Stars made of matter that has an even ...
MASSACHUSETTS INSTITUTE OF TECHNOLOGY
... (c) Assuming that the moment of inertia is that of a uniform sphere when the collapse begins, and that the moment inertia is that of a uniform disk when the collapse ends, determine the rotational velocity at 100 AU when the collapse stops. (d) After the collapse has stopped, calculate the time requ ...
... (c) Assuming that the moment of inertia is that of a uniform sphere when the collapse begins, and that the moment inertia is that of a uniform disk when the collapse ends, determine the rotational velocity at 100 AU when the collapse stops. (d) After the collapse has stopped, calculate the time requ ...
GALEX UV Light-curves of M-Dwarf Flare Stars: THE FLARING UV
... • The magnetic field-lines of a star stretch up into their outer atmosphere - the corona - in loop-like structures • When adjacent magnetic field lines “re-connect” (probably due to disturbances within the stellar interior) they release energy in the form of electrons that gyrate down the field line ...
... • The magnetic field-lines of a star stretch up into their outer atmosphere - the corona - in loop-like structures • When adjacent magnetic field lines “re-connect” (probably due to disturbances within the stellar interior) they release energy in the form of electrons that gyrate down the field line ...
Chapter 10 Late evolution of low- and intermediate
... shown in Fig. 10.4, the surface 12 C abundance increases after every dredge-up episode and thus gradually increases, until it exceeds the 16 O abundance after 1.3 × 106 yr. The star has thus turned into a carbon star, with a surface number ratio of C/O > 1. Besides carbon, AGB stars are considered t ...
... shown in Fig. 10.4, the surface 12 C abundance increases after every dredge-up episode and thus gradually increases, until it exceeds the 16 O abundance after 1.3 × 106 yr. The star has thus turned into a carbon star, with a surface number ratio of C/O > 1. Besides carbon, AGB stars are considered t ...
Red Supergiants as the Progenitors of Type IIP Supernova
... While for a 2D model with explosion energy around 1.8× 1051 erg the Si and Ni containing structures still move with nearly 4000 km s-1 (oxygen has velocities up to even 5000 km s-1) at 300 s, a strong deceleration occurs when the metal clumps enter the relatively dense He-shell that forms after the ...
... While for a 2D model with explosion energy around 1.8× 1051 erg the Si and Ni containing structures still move with nearly 4000 km s-1 (oxygen has velocities up to even 5000 km s-1) at 300 s, a strong deceleration occurs when the metal clumps enter the relatively dense He-shell that forms after the ...
Mass loss in semi-detached binaries
... In general, the star expands and the effective temperature drops which causes it to move towards right into the giant and subgiant region of the H-R-diagram. There is also an increase in luminosity due to the increase in mean molecular weight caused by the conversion of hydrogen into helium in the c ...
... In general, the star expands and the effective temperature drops which causes it to move towards right into the giant and subgiant region of the H-R-diagram. There is also an increase in luminosity due to the increase in mean molecular weight caused by the conversion of hydrogen into helium in the c ...