Explore the Galaxy - Museum of Science, Boston
... the planets, moons, asteroids, comets and dwarf planets and their properties. Outside the solar system, interstellar space and phenomena like nebulae, star clusters, and exoplanets are explored. On a larger scale, we discuss the Milky Way Galaxy and its major components, such as the spiral arms, cen ...
... the planets, moons, asteroids, comets and dwarf planets and their properties. Outside the solar system, interstellar space and phenomena like nebulae, star clusters, and exoplanets are explored. On a larger scale, we discuss the Milky Way Galaxy and its major components, such as the spiral arms, cen ...
Gamma - Ray Observations of Olaf Reimer
... gamma-ray binaries as compact PWN • Interpretation as pulsar / stellar wind interaction explains similarities between VHE emitting binaries. • VHE emission occurs close to pulsar/star (γγ absorption should modulate TeV flux in LS 5039). • Large scale emission can be explained by comet-like shocked m ...
... gamma-ray binaries as compact PWN • Interpretation as pulsar / stellar wind interaction explains similarities between VHE emitting binaries. • VHE emission occurs close to pulsar/star (γγ absorption should modulate TeV flux in LS 5039). • Large scale emission can be explained by comet-like shocked m ...
TDE in the XMM-Newton slew survey
... focussing on the ones found in the XMM slew • Where do X-rays in TDE come from? • Galaxy types • Latest results ...
... focussing on the ones found in the XMM slew • Where do X-rays in TDE come from? • Galaxy types • Latest results ...
Chapter 18 The Bizarre Stellar Graveyard What is a white dwarf
... electrons must move at nearly the speed of light • Because nothing can move faster than light, a white dwarf cannot be more massive than 1.4MSun, the white dwarf limit (or Chandrasekhar limit) ...
... electrons must move at nearly the speed of light • Because nothing can move faster than light, a white dwarf cannot be more massive than 1.4MSun, the white dwarf limit (or Chandrasekhar limit) ...
Stellar Evolution: The Lives of Stars
... “die” various deaths based on their mass. It is the crushing force of gravity on such great mass that “sparks” the process of nuclear fusion. Stars lead short lives if they are massive and long lives if not. Their “deaths” also depend on their original mass. Recall that nuclear fusion is an outward ...
... “die” various deaths based on their mass. It is the crushing force of gravity on such great mass that “sparks” the process of nuclear fusion. Stars lead short lives if they are massive and long lives if not. Their “deaths” also depend on their original mass. Recall that nuclear fusion is an outward ...
29.3-stellar-evolution
... The density and temp in a star increase toward the center, where energy is generated by nuclear fusion. Stellar Evolution As long as a star is changing hydrogen into helium, nuclear fusion, it will be a main sequence star. Star formation The formation of a star begins with a cloud of dust and ...
... The density and temp in a star increase toward the center, where energy is generated by nuclear fusion. Stellar Evolution As long as a star is changing hydrogen into helium, nuclear fusion, it will be a main sequence star. Star formation The formation of a star begins with a cloud of dust and ...
Einstein
... Chandrasekhar got his solution based on the equation of state for an ideal Fermi gas ...
... Chandrasekhar got his solution based on the equation of state for an ideal Fermi gas ...
WEEK 8: CSI UCSC: ASTRO EDITION SOLUTIONS This week you
... (1) Compare Types I and II supernovae. What kinds of objects explode and what are their explosion mechanisms? There are two main types. The first one is Type Ia supernova, which comes from a white dwarf in a binary system with another star. A white dwarf may steal material from the companion star, a ...
... (1) Compare Types I and II supernovae. What kinds of objects explode and what are their explosion mechanisms? There are two main types. The first one is Type Ia supernova, which comes from a white dwarf in a binary system with another star. A white dwarf may steal material from the companion star, a ...
Stars & Galaxies
... Small and medium stars become red giants and then white dwarfs. Their outer layers expand to become red giants. Eventually, the outer parts grow bigger still and drift out into space. The blue white hot core is left behind causing a white dwarf. When there is no more energy it becomes a black dwarf. ...
... Small and medium stars become red giants and then white dwarfs. Their outer layers expand to become red giants. Eventually, the outer parts grow bigger still and drift out into space. The blue white hot core is left behind causing a white dwarf. When there is no more energy it becomes a black dwarf. ...
Solutions to test #2 taken on Tuesday
... 2. (15) Millions, Billions or One. This is an “order of magnitude” question. Pick the number (the order of magnitude) that is closest for each. a) _millions_The temperature in the core of the Sun. b) ___one__ The size of a typical black hole’s event horizon (in kilometers) created in the death of a ...
... 2. (15) Millions, Billions or One. This is an “order of magnitude” question. Pick the number (the order of magnitude) that is closest for each. a) _millions_The temperature in the core of the Sun. b) ___one__ The size of a typical black hole’s event horizon (in kilometers) created in the death of a ...
31 October: Supernovae and Neutron Stars
... a neutron star • The remnant after the explosion of a massive star • An object having the mass of the Sun (or more) but in an object with the diameter of Iowa City! • An equivalent to the Chandrasekhar mass (largest possible mass of a neutron star) • Do they exist? ...
... a neutron star • The remnant after the explosion of a massive star • An object having the mass of the Sun (or more) but in an object with the diameter of Iowa City! • An equivalent to the Chandrasekhar mass (largest possible mass of a neutron star) • Do they exist? ...
Astronomy 102, Spring 2003 Solutions to Review Problems
... the pulsar could just not be pointing in the right direction for us to see them, or the supernova could have been from a hugely massive star that left behind a black hole rather than a pulsar. Sometimes there’s just no way to know. We observe supernovae now where the type is in doubt; the lightcurve ...
... the pulsar could just not be pointing in the right direction for us to see them, or the supernova could have been from a hugely massive star that left behind a black hole rather than a pulsar. Sometimes there’s just no way to know. We observe supernovae now where the type is in doubt; the lightcurve ...
Black Hole
... gas back into the interstellar medium. This is a total of more than 1 billion M or more than 1 % of the mass of the Galaxy. ...
... gas back into the interstellar medium. This is a total of more than 1 billion M or more than 1 % of the mass of the Galaxy. ...
Exploring the Planet Forming Environments of Young Suns
... Young RV Planets to Date • Setiawan et al. (2007) identified long period (852d) planet around 100 Myr old star HD 70573 • In 2008 team claimed detection of a 10MJ, 10 Myr old planet @ TW Hya ...
... Young RV Planets to Date • Setiawan et al. (2007) identified long period (852d) planet around 100 Myr old star HD 70573 • In 2008 team claimed detection of a 10MJ, 10 Myr old planet @ TW Hya ...
main characteristics of the emission from elliptical galaxies
... Elliptical galaxies are one of the most characteristic objects we can nd in the sky. In order to unveil their properties, such as their structure or chemical composition, one must study their spectral emission. In fact they seem to behave rather dierently when observed with dierent eyes. This is ...
... Elliptical galaxies are one of the most characteristic objects we can nd in the sky. In order to unveil their properties, such as their structure or chemical composition, one must study their spectral emission. In fact they seem to behave rather dierently when observed with dierent eyes. This is ...
X-ray Emission Line Profile Diagnostics of Hot Star Winds
... But, hot star winds are not steady-state: They display lots of time variability. 16 days of UV spectra of z Pup. The color plot is the ratio of each spectrum to the mean spectrum (bottom). Cyclical and stochastic variability is seen in most hot stars’ winds ...
... But, hot star winds are not steady-state: They display lots of time variability. 16 days of UV spectra of z Pup. The color plot is the ratio of each spectrum to the mean spectrum (bottom). Cyclical and stochastic variability is seen in most hot stars’ winds ...
AST101 Lecture 20 The Ecology of the Galaxy
... • About 1010 years old • 105 - 106 stars • Radius ~ 10 light years • Most massive star: ~ 1 solar mass • ~150 globular clusters known in Milky Way ...
... • About 1010 years old • 105 - 106 stars • Radius ~ 10 light years • Most massive star: ~ 1 solar mass • ~150 globular clusters known in Milky Way ...
GLY 1001 Earth Science Name:__Answers
... Pulsating variable - A variable star that pulsates in size and luminosity. Red giant – A large, cool star of high luminosity, a star occupying the upper-right portion of the Hertzsprung-Russell Diagram. Reflection nebula – A relatively dense dust cloud in interstellar space that is illuminated by st ...
... Pulsating variable - A variable star that pulsates in size and luminosity. Red giant – A large, cool star of high luminosity, a star occupying the upper-right portion of the Hertzsprung-Russell Diagram. Reflection nebula – A relatively dense dust cloud in interstellar space that is illuminated by st ...
The Stellar Graveyard
... loss during the various phases of stellar evolution following hydrogen core exhaustion. Measuring the current mass of a white dwarf, therefore, does not indicate what its initial mass was. A 0.5 solar mass white dwarf could have easily started out life as a 10 solar mass main sequence star. A white ...
... loss during the various phases of stellar evolution following hydrogen core exhaustion. Measuring the current mass of a white dwarf, therefore, does not indicate what its initial mass was. A 0.5 solar mass white dwarf could have easily started out life as a 10 solar mass main sequence star. A white ...
Review: How does a star`s mass determine its life story?
... One famous X-ray binary with a likely black hole is in the constellation Cygnus. ...
... One famous X-ray binary with a likely black hole is in the constellation Cygnus. ...
Supernovae
... Neutrinos carry energy out of the star and provide momentum through collisions to throw off material. Or they heat the material so that it expands. They have no mass (like photons) and can traverse large depths without being absorbed. ...
... Neutrinos carry energy out of the star and provide momentum through collisions to throw off material. Or they heat the material so that it expands. They have no mass (like photons) and can traverse large depths without being absorbed. ...
lecture20
... collapse. • As more gas fell in, it’s potential energy was converted into thermal energy. • Eventually the in-falling gas was hot enough to ignite nuclear fusion in the core. • Gas that continued to fall in helped to establish gravitational equilibrium with the pressure generated in the core. ...
... collapse. • As more gas fell in, it’s potential energy was converted into thermal energy. • Eventually the in-falling gas was hot enough to ignite nuclear fusion in the core. • Gas that continued to fall in helped to establish gravitational equilibrium with the pressure generated in the core. ...
Black Hole Binaries in Quiescence
... • XRB: assume that supply of mass is constant, and that variability is due to accretion flow instabilities • AGN: assume significant changes in mass supply (tidal disruption etc) ...
... • XRB: assume that supply of mass is constant, and that variability is due to accretion flow instabilities • AGN: assume significant changes in mass supply (tidal disruption etc) ...
Dynamics of nuclear burning during type-I X-ray bursts 1. 2. 3.
... 1. Overview of X-ray burst phenomena 2. Effects of rotation and structure of burning fronts 3. Propagation of burning on a sphere 4. Burning dynamics in magnetic fields -- application to SAX J1808 5. Conclusions and connection to observations ...
... 1. Overview of X-ray burst phenomena 2. Effects of rotation and structure of burning fronts 3. Propagation of burning on a sphere 4. Burning dynamics in magnetic fields -- application to SAX J1808 5. Conclusions and connection to observations ...
Astrophysical X-ray source
Astrophysical X-ray sources are astronomical objects with physical properties which result in the emission of X-rays.There are a number of types of astrophysical objects which emit X-rays, from galaxy clusters, through black holes in active galactic nuclei (AGN) to galactic objects such as supernova remnants, stars, and binary stars containing a white dwarf (cataclysmic variable stars and super soft X-ray sources), neutron star or black hole (X-ray binaries). Some solar system bodies emit X-rays, the most notable being the Moon, although most of the X-ray brightness of the Moon arises from reflected solar X-rays. A combination of many unresolved X-ray sources is thought to produce the observed X-ray background. The X-ray continuum can arise from bremsstrahlung, either magnetic or ordinary Coulomb, black-body radiation, synchrotron radiation, inverse Compton scattering of lower-energy photons be relativistic electrons, knock-on collisions of fast protons with atomic electrons, and atomic recombination, with or without additional electron transitions.Furthermore, celestial entities in space are discussed as celestial X-ray sources. The origin of all observed astronomical X-ray sources is in, near to, or associated with a coronal cloud or gas at coronal cloud temperatures for however long or brief a period.