NAME
... ____ 20. What type of standard candle is used to determine distances to globular clusters? a. O-type main-sequence stars b. Cepheid variable stars c. T Tauri stars d. Type I supernovae e. RR Lyrae stars ____ 21. By comparing globular clusters, you find that Cluster A’s RR Lyrae stars are 100 times f ...
... ____ 20. What type of standard candle is used to determine distances to globular clusters? a. O-type main-sequence stars b. Cepheid variable stars c. T Tauri stars d. Type I supernovae e. RR Lyrae stars ____ 21. By comparing globular clusters, you find that Cluster A’s RR Lyrae stars are 100 times f ...
Atoms, X-rays and Synchrotron Radiation
... - no photoelectrons are emitted when the incident light has a frequency below the threshold, - the maximum kinetic energy of the photoelectrons increases with the frequency of the incident light, - the maximum kinetic energy of the photoelectrons is independent of the intensity of the incident light ...
... - no photoelectrons are emitted when the incident light has a frequency below the threshold, - the maximum kinetic energy of the photoelectrons increases with the frequency of the incident light, - the maximum kinetic energy of the photoelectrons is independent of the intensity of the incident light ...
Structure of Neutron Stars
... However, then in 2007 at a conference the authors announced that the result was incorrect. Actually, the initial value was 2.1+/-0.2 (1 sigma error). New result: 1.26 +/- 0.14 solar [Nice et al. 2008, Proc. of the conf. “40 Years of pulsars”] 3. PSR B1516+02B in a globular cluster. M~2 solar (M>1.72 ...
... However, then in 2007 at a conference the authors announced that the result was incorrect. Actually, the initial value was 2.1+/-0.2 (1 sigma error). New result: 1.26 +/- 0.14 solar [Nice et al. 2008, Proc. of the conf. “40 Years of pulsars”] 3. PSR B1516+02B in a globular cluster. M~2 solar (M>1.72 ...
Unit 9E.1 The Life Cycle of Stars17213
... stage of its life cycle, an average star is classified as a white dwarf. A white dwarf is the small, hot, leftover center of a red giant. ...
... stage of its life cycle, an average star is classified as a white dwarf. A white dwarf is the small, hot, leftover center of a red giant. ...
2.1c Notes - Vanderbilt University
... turned into neutrons leading to the formation of a “neutron star”, and in addition lots of highenergy neutrinos will be produced. The “neutrino wind” drives the supernova explosion of the star. Apart from Hubble Space Telescope pictures of the supernova explosion in the visible part of the light spe ...
... turned into neutrons leading to the formation of a “neutron star”, and in addition lots of highenergy neutrinos will be produced. The “neutrino wind” drives the supernova explosion of the star. Apart from Hubble Space Telescope pictures of the supernova explosion in the visible part of the light spe ...
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 ...
Black Holes
... A collapsing object becomes a black hole when the escape velocity from its surface exceeds the speed of light. The event horizon is not a physical surface, just a distance from the center. Nothing can escape from within the event horizon because nothing can go faster than light. The event horizon ge ...
... A collapsing object becomes a black hole when the escape velocity from its surface exceeds the speed of light. The event horizon is not a physical surface, just a distance from the center. Nothing can escape from within the event horizon because nothing can go faster than light. The event horizon ge ...
AST 101 INTRODUCTION TO ASTRONOMY SPRING 2008
... B. After the probe passes through the event horizon you would see its image frozen, stuck at the place and time it crossed over C. The lights on the probe would appear to change color, becoming redder D. The probe’s clock would appear to slow down E. Once inside the event horizon, you would see the ...
... B. After the probe passes through the event horizon you would see its image frozen, stuck at the place and time it crossed over C. The lights on the probe would appear to change color, becoming redder D. The probe’s clock would appear to slow down E. Once inside the event horizon, you would see the ...
Version0 Answers
... clock) near a black hole, and watch it fall in. Which of the following statements is NOT TRUE about what you would see? A. The probe’s clock would appear to slow down B. After the probe passes through the event horizon you would see its image frozen, stuck at the place and time it crossed over C. On ...
... clock) near a black hole, and watch it fall in. Which of the following statements is NOT TRUE about what you would see? A. The probe’s clock would appear to slow down B. After the probe passes through the event horizon you would see its image frozen, stuck at the place and time it crossed over C. On ...
Final Review Sheet
... by mass (75% by radius). In the outer parts energy is transported by convection. Sunspots are regions on the surface of the sun characterized by lower temperature (by about 1000 K) than their surroundings and have strong magnetic fields (1000 Gauss). They generally come in pairs with opposite magnet ...
... by mass (75% by radius). In the outer parts energy is transported by convection. Sunspots are regions on the surface of the sun characterized by lower temperature (by about 1000 K) than their surroundings and have strong magnetic fields (1000 Gauss). They generally come in pairs with opposite magnet ...
D109-08x
... luminosity of these knots (with sizes of 2-5 kpc) was measured to be MV ~ -16.2 (substantially brighter than most dwarf galaxies) with individual luminosities ranging from -15 < MV < -17. Moreover, their colors were extremely blue in (V-I) averaging 0.15 +/- 0.06. Thus, these knots have properties s ...
... luminosity of these knots (with sizes of 2-5 kpc) was measured to be MV ~ -16.2 (substantially brighter than most dwarf galaxies) with individual luminosities ranging from -15 < MV < -17. Moreover, their colors were extremely blue in (V-I) averaging 0.15 +/- 0.06. Thus, these knots have properties s ...
Astronomy 1001/1005 Final Exam (250 points)
... Spiral Galaxies are easily identified by their flat disk, usually containing well-defined spiral arms as well as gas and dust. They also have a central spheroidal bulge and are surrounded by a spheroidal halo containing globular clusters. Elliptical Galaxies are simple spheroidal collections of star ...
... Spiral Galaxies are easily identified by their flat disk, usually containing well-defined spiral arms as well as gas and dust. They also have a central spheroidal bulge and are surrounded by a spheroidal halo containing globular clusters. Elliptical Galaxies are simple spheroidal collections of star ...
The life-cycle of stars - Young Scientists Journal
... Stars with more than 10 solar masses become red supergiants, after burning all their hydrogen,during the stage when they fuse helium into carbon. These supergiants have relatively cool surface temperatures (3500-4500 K) and radii between 200 and 800 times the Sun’s radius. As the helium turns into c ...
... Stars with more than 10 solar masses become red supergiants, after burning all their hydrogen,during the stage when they fuse helium into carbon. These supergiants have relatively cool surface temperatures (3500-4500 K) and radii between 200 and 800 times the Sun’s radius. As the helium turns into c ...
Lecture Notes – Stars
... This material gradually spirals in towards the compact object, creating an accretion disk, which is heated and emits X-rays. Many X-ray binaries are known. The masses of the two components can be measured using Kepler’s third law. In most cases, the masses are consistent with neutron stars. In a fe ...
... This material gradually spirals in towards the compact object, creating an accretion disk, which is heated and emits X-rays. Many X-ray binaries are known. The masses of the two components can be measured using Kepler’s third law. In most cases, the masses are consistent with neutron stars. In a fe ...
Sirius Astronomer - Orange County Astronomers
... forces within them are powerful enough to form new elements (in fact, almost all of the elements with a mass greater than Helium were made in supernovae), and the shock waves they produce help to start the process of new stellar formation. Seeing a supernova is not that easy. It is estimated from su ...
... forces within them are powerful enough to form new elements (in fact, almost all of the elements with a mass greater than Helium were made in supernovae), and the shock waves they produce help to start the process of new stellar formation. Seeing a supernova is not that easy. It is estimated from su ...
AMUSE-Virgo AGN Multi-wavelength Survey
... Targets 100 early type galaxies which compose the HST ACS Virgo Cluster Survey (ACSVCS, Cote’ et al 04) - 84 new targets with Chandra ACIS-S (454 ksec; PI: Treu) + 16 archival - 57 new targets with Spitzer MIPS (9.5 hr) + 43 archival - HST ACS archival data (100 orbits) - VLA, in progress (with D. A ...
... Targets 100 early type galaxies which compose the HST ACS Virgo Cluster Survey (ACSVCS, Cote’ et al 04) - 84 new targets with Chandra ACIS-S (454 ksec; PI: Treu) + 16 archival - 57 new targets with Spitzer MIPS (9.5 hr) + 43 archival - HST ACS archival data (100 orbits) - VLA, in progress (with D. A ...
Molecular Gas in Nearby Dwarf Galaxies:
... Follow up of 30+ galaxies mapped using BIMA Fabian Walter’s OVRO sample ...
... Follow up of 30+ galaxies mapped using BIMA Fabian Walter’s OVRO sample ...
Lecture 29: Ellipticals and Irregulars
... Integrated light/spectra Emission lines, particularly from neutral hydrogen and molecular gas. ...
... Integrated light/spectra Emission lines, particularly from neutral hydrogen and molecular gas. ...
Recent advances in star
... small-scale features and their properties detected by Girart and collaborators. In contrast to these theoretical speculations, it was especially refreshing for everyone at the meeting to hear Derek Ward-Thompson’s (Cardiff) review of the observed initial conditions for low-mass star formation. This ...
... small-scale features and their properties detected by Girart and collaborators. In contrast to these theoretical speculations, it was especially refreshing for everyone at the meeting to hear Derek Ward-Thompson’s (Cardiff) review of the observed initial conditions for low-mass star formation. This ...
Galaxies - science1d
... •The most distant galaxies are 15 million ly away •When light left them, the ...
... •The most distant galaxies are 15 million ly away •When light left them, the ...
Which Stars Form Black Holes and Neutron Stars?
... would have implications for both the Galactic population of these unusual neutron stars, and for the evolution and deaths of massive stars. First, if magnetars only descend from massive progenitors, then they would be expected to be rare compared to radio pulsars [25]. For a standard initial mass fu ...
... would have implications for both the Galactic population of these unusual neutron stars, and for the evolution and deaths of massive stars. First, if magnetars only descend from massive progenitors, then they would be expected to be rare compared to radio pulsars [25]. For a standard initial mass fu ...
non-thermal physics of galaxy clusters
... The origin of the intracluster non-thermal component observed at radio wavelengths is one of the main open questions of current cluster studies. Magnetic fields at the observed intensity level (≈ 1 µGauss) could result from amplification of seed fields through adiabatic compression, turbulence and s ...
... The origin of the intracluster non-thermal component observed at radio wavelengths is one of the main open questions of current cluster studies. Magnetic fields at the observed intensity level (≈ 1 µGauss) could result from amplification of seed fields through adiabatic compression, turbulence and s ...
21. The Milky Way Galaxy
... Also, squeezing of clouds initiates collapse within them => star formation. Bright young massive stars live and die in spiral arms. Emission nebulae mostly in spiral arms. So arms always contain same types of objects, but individual objects come and go. ...
... Also, squeezing of clouds initiates collapse within them => star formation. Bright young massive stars live and die in spiral arms. Emission nebulae mostly in spiral arms. So arms always contain same types of objects, but individual objects come and go. ...
Galaxies - Center for Astrostatistics
... Tauri stars, open clusters, supernova remnants and X-ray binaries. The maps below show the disk at infrared, 21-cm hydrogen, CO molecules, and visible light. There is an intricate relationship between the interstellar medium and stars in the Galactic disk. Star are born in cold molecular clouds., or ...
... Tauri stars, open clusters, supernova remnants and X-ray binaries. The maps below show the disk at infrared, 21-cm hydrogen, CO molecules, and visible light. There is an intricate relationship between the interstellar medium and stars in the Galactic disk. Star are born in cold molecular clouds., or ...
Astronomy 110G Review Sheet for Exam #3 The
... behind. White dwarves are supported by their electrons being packed as closely together as possible and are about 100 times smaller than the Sun. Above about 1.44 solar masses gravity can “squeeze” the electrons into the protons to form neutrons. Resulting neutron stars (sometimes observed as pulsar ...
... behind. White dwarves are supported by their electrons being packed as closely together as possible and are about 100 times smaller than the Sun. Above about 1.44 solar masses gravity can “squeeze” the electrons into the protons to form neutrons. Resulting neutron stars (sometimes observed as pulsar ...
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.