Lec11_ch13_blackholes
... • Leads to profound conclusions! – length contraction of moving objects – time dilation of moving clocks – mass of an object increases with speed, requiring infinite energy to reach the speed of light – equivalence of mass and energy: E=mc2 – led to the concept of an integrated “spacetime” which is ...
... • Leads to profound conclusions! – length contraction of moving objects – time dilation of moving clocks – mass of an object increases with speed, requiring infinite energy to reach the speed of light – equivalence of mass and energy: E=mc2 – led to the concept of an integrated “spacetime” which is ...
Thermal emission and internal heating processes in millisecond
... • Observed UV emission of PSR J0437-4715 may be due to rotochemical heating • The same emission can be used to constrain |dG/dt|: – competitive with best existing constraints if fast cooling processes could be ruled out ...
... • Observed UV emission of PSR J0437-4715 may be due to rotochemical heating • The same emission can be used to constrain |dG/dt|: – competitive with best existing constraints if fast cooling processes could be ruled out ...
– 1 – 1. Feedback From The First Stars
... b) A new perspective on the epoch of reionization perhaps can be obtained using GRBs to reach higher redshift. The prompt X-ray and γ-ray emission of GRBs is not attenuated by gas or dust, and hence GRBs should in principle be detected from the reionization era. Furthermore GRBs at maximum are very ...
... b) A new perspective on the epoch of reionization perhaps can be obtained using GRBs to reach higher redshift. The prompt X-ray and γ-ray emission of GRBs is not attenuated by gas or dust, and hence GRBs should in principle be detected from the reionization era. Furthermore GRBs at maximum are very ...
Discussion Session A: “Evidence”
... instantaneous LAGN • B) Correla8on of SFR and average LAGN (or BH accre8on rate) • C) Increased AGN frac'on in SF galaxies • D) Radio AGN are associated with quiescent galaxies/high mass halos/hot a ...
... instantaneous LAGN • B) Correla8on of SFR and average LAGN (or BH accre8on rate) • C) Increased AGN frac'on in SF galaxies • D) Radio AGN are associated with quiescent galaxies/high mass halos/hot a ...
1. INTRODUCTION
... as these stars often show several distinct stochastic events. We have focused our analysis on young, active stars that do not display rotationally modulated light curves and that can be considered as single X-ray sources. Some stars in the sample are detected or known binary systems, in which only o ...
... as these stars often show several distinct stochastic events. We have focused our analysis on young, active stars that do not display rotationally modulated light curves and that can be considered as single X-ray sources. Some stars in the sample are detected or known binary systems, in which only o ...
Weighing Ultracompact Dwarf Galaxies in the Fornax Cluster
... are consistent with those expected for pure stellar populations. No dark matter contribution is needed. Thus, these UCDs seem to be the result of star-cluster formation processes within galaxies, rather than being compact dwarf galaxies formed in dark-matter halos. Dwarf galaxies have only been exte ...
... are consistent with those expected for pure stellar populations. No dark matter contribution is needed. Thus, these UCDs seem to be the result of star-cluster formation processes within galaxies, rather than being compact dwarf galaxies formed in dark-matter halos. Dwarf galaxies have only been exte ...
The role of black holes in galaxy formation and evolution
... much of the cluster core. These clusters are called ‘cool-core’ clusters because T decreases towards the centre. However, cool-core clusters are not ‘cold core’ clusters: the temperature drops towards the centre by only a factor of three. From the absence or weakness of the soft X-ray line Fe XVII, ...
... much of the cluster core. These clusters are called ‘cool-core’ clusters because T decreases towards the centre. However, cool-core clusters are not ‘cold core’ clusters: the temperature drops towards the centre by only a factor of three. From the absence or weakness of the soft X-ray line Fe XVII, ...
ACTIVE GALAXIES
... • Head-tail radio galaxies arise when jets are bent by the ram-pressure of gas as the host galaxy moves through it. • For powerful sources only one jet is seen: this is because of RELATIVISTIC DOPPER BOOSTING: the approaching jet appears MUCH brighter than an intrinsically equal receding jet since m ...
... • Head-tail radio galaxies arise when jets are bent by the ram-pressure of gas as the host galaxy moves through it. • For powerful sources only one jet is seen: this is because of RELATIVISTIC DOPPER BOOSTING: the approaching jet appears MUCH brighter than an intrinsically equal receding jet since m ...
Gas IN - STScI
... For ETGs, the ability to sustain a corona of hot, X-ray emitting gas could have played a key role in quenching their past star formation history. An halo of hot gas can indeed act as an effective shield against the acquisition of cold gas and can quickly absorb any stellar mass loss material. But wh ...
... For ETGs, the ability to sustain a corona of hot, X-ray emitting gas could have played a key role in quenching their past star formation history. An halo of hot gas can indeed act as an effective shield against the acquisition of cold gas and can quickly absorb any stellar mass loss material. But wh ...
SUMMARY OF KEY CONCEPTS: GALAXIES AND COSMOLOGY
... and gas. Dark energy – unseen `substance’ that appears to be causing the rate of expansion of the Universe to be accelerating (the opposite of what gravity is expected to do). In addition to the evidence from spiral galaxy rotation curves, additional evidence for the existence of dark matter comes f ...
... and gas. Dark energy – unseen `substance’ that appears to be causing the rate of expansion of the Universe to be accelerating (the opposite of what gravity is expected to do). In addition to the evidence from spiral galaxy rotation curves, additional evidence for the existence of dark matter comes f ...
Chapter15 (with interactive links)
... The Milky Way offers clues to galaxy formation. The stars in globular clusters in the halo have some heavy elements, so at least one prior generation of stars must have existed. Halo objects were formed before interstellar gas was all concentrated into the disk. Later star formation has been ...
... The Milky Way offers clues to galaxy formation. The stars in globular clusters in the halo have some heavy elements, so at least one prior generation of stars must have existed. Halo objects were formed before interstellar gas was all concentrated into the disk. Later star formation has been ...
Chapter 10: The Sun-
... • Reasonable rates: few tens per year at >1 Hz • Unique probe of dense cluster star formation ...
... • Reasonable rates: few tens per year at >1 Hz • Unique probe of dense cluster star formation ...
Get ready for quiz # 7
... 14.6 The Mass of the Milky Way Galaxy The orbital speed of an object depends only on the amount of mass between it and the galactic center. ...
... 14.6 The Mass of the Milky Way Galaxy The orbital speed of an object depends only on the amount of mass between it and the galactic center. ...
The Evolution of Galaxy - Tufts Institute of Cosmology
... X-RAY IMAGES of Coma (left) and Virgo (right) clusters show the hot intergalactic gas that dominates the luminous part of these structures. The gas in Coma has a more regular shape than that in Virgo, suggesting that the cluster has reached a more advanced stage of formation. Both clusters are surro ...
... X-RAY IMAGES of Coma (left) and Virgo (right) clusters show the hot intergalactic gas that dominates the luminous part of these structures. The gas in Coma has a more regular shape than that in Virgo, suggesting that the cluster has reached a more advanced stage of formation. Both clusters are surro ...
mam.mwism
... stars as the disk, and very little gas and dust. We can’t detect halos of other galaxies. Nuclear bulge has radius of 2 kpc and contains little gas and dust. ...
... stars as the disk, and very little gas and dust. We can’t detect halos of other galaxies. Nuclear bulge has radius of 2 kpc and contains little gas and dust. ...
Physica 133-11f: Sample Final Exam Here are sample questions for
... A) young, red, and dim and have fewer heavy elements. B) old, red, and bright and have fewer heavy elements. C) young, blue, and bright and have much more heavy element material. D) old, red, and dim and have much more heavy element material. E) old, red, and dim and have fewer heavy elements. ...
... A) young, red, and dim and have fewer heavy elements. B) old, red, and bright and have fewer heavy elements. C) young, blue, and bright and have much more heavy element material. D) old, red, and dim and have much more heavy element material. E) old, red, and dim and have fewer heavy elements. ...
Chandra HETGS Multiphase Spectroscopy Of The Young
... its X-ray flux modulated on the star’s 15 day rotation period (Gagné et al. 1997). Hard, time-variable X-ray emission is not expected from O stars because they do not possess an outer convective envelope to drive a solar-type magnetic dynamo. Rather, the detection of a variable longitudinal magneti ...
... its X-ray flux modulated on the star’s 15 day rotation period (Gagné et al. 1997). Hard, time-variable X-ray emission is not expected from O stars because they do not possess an outer convective envelope to drive a solar-type magnetic dynamo. Rather, the detection of a variable longitudinal magneti ...
PDF Full-text
... UV and Lyman-α fluxes. This paper summarizes where these observed fluxes are available and, in the absence of observations, how these fluxes may be estimated. EUV and X-ray radiation from host star chromospheres and coronae play a different role in the outer atmospheres of close-in hot Jupiters, min ...
... UV and Lyman-α fluxes. This paper summarizes where these observed fluxes are available and, in the absence of observations, how these fluxes may be estimated. EUV and X-ray radiation from host star chromospheres and coronae play a different role in the outer atmospheres of close-in hot Jupiters, min ...
1: Properties of Pulsars
... The following animations demonstrate that pulsars concentrate so much mass that they are almost black holes. In fact, if a pulsar would have only twice as much mass, a collapse to a black hole could probably not be prevented. Both animations are based on correct calculations in the frame work of gen ...
... The following animations demonstrate that pulsars concentrate so much mass that they are almost black holes. In fact, if a pulsar would have only twice as much mass, a collapse to a black hole could probably not be prevented. Both animations are based on correct calculations in the frame work of gen ...
Which of the following is not a characteristic of the stars of the disk
... Please indicate the best answer to the following questions on the answer sheet provided. 1. Which of the following is not a characteristic of the stars of the disk component of our galaxy? a. circular orbits, b. randomly inclined orbits, c. higher metal abundance d. young stars, 2. The mass of a sin ...
... Please indicate the best answer to the following questions on the answer sheet provided. 1. Which of the following is not a characteristic of the stars of the disk component of our galaxy? a. circular orbits, b. randomly inclined orbits, c. higher metal abundance d. young stars, 2. The mass of a sin ...
ppt - SLAC
... 2. Atmospheric pressure depends on the star's surface gravity and so, roughly, on its size —a giant, dwarf, or in between. The size and surface brightness yield the star's luminosity and often its evolutionary status (young, middle-aged, or nearing death). Apparent brightness then gives an idea of t ...
... 2. Atmospheric pressure depends on the star's surface gravity and so, roughly, on its size —a giant, dwarf, or in between. The size and surface brightness yield the star's luminosity and often its evolutionary status (young, middle-aged, or nearing death). Apparent brightness then gives an idea of t ...
HST Paα Survey of the Galactic Center – Seeking the Missing
... the Padova stellar evolutionary tracks in the right panel of Fig. 2. The F190N contours are calculated from the ATLAS 9 atmosphere model and corrected for the distance and extinction (AV = 31.1). As shown by the figure, most of the detected sources should be red giants and AGB stars. Only Main Seque ...
... the Padova stellar evolutionary tracks in the right panel of Fig. 2. The F190N contours are calculated from the ATLAS 9 atmosphere model and corrected for the distance and extinction (AV = 31.1). As shown by the figure, most of the detected sources should be red giants and AGB stars. Only Main Seque ...
The Milky Way-Pulsars and Isolated Neutron Stars
... from the Moon2 , they launched an Aerobee rocket on 12 June 1962 from White Sands (New Mexico) with three Geiger counters as payload, each having a ∼ 100◦ field of view and an effective collecting area of about 10 cm2 (Giacconi 1974). The experiment detected X-rays not from the Moon but from a sourc ...
... from the Moon2 , they launched an Aerobee rocket on 12 June 1962 from White Sands (New Mexico) with three Geiger counters as payload, each having a ∼ 100◦ field of view and an effective collecting area of about 10 cm2 (Giacconi 1974). The experiment detected X-rays not from the Moon but from a sourc ...
A Massive Molecular Gas Reservoir in the z= 5.3 Submillimeter
... <4 kpc and likely consists of a ‘diffuse’, low-excitation component, containing (at least) 1/3 of the gas mass (depending on the relative conversion factor αCO ), and a ‘dense’, high-excitation component, containing ∼2/3 of the mass. The likely presence of a substantial diffuse component besides hig ...
... <4 kpc and likely consists of a ‘diffuse’, low-excitation component, containing (at least) 1/3 of the gas mass (depending on the relative conversion factor αCO ), and a ‘dense’, high-excitation component, containing ∼2/3 of the mass. The likely presence of a substantial diffuse component besides hig ...
A new isolated dSph galaxy near the Local Group
... initial mass function (IMF). The synthetic diagrams were altered by the same incompleteness, crowding effects and photometric systematics as those determined for the observations using artificial star experiments. A full description of the details of our approach and the STARPROBE software are given ...
... initial mass function (IMF). The synthetic diagrams were altered by the same incompleteness, crowding effects and photometric systematics as those determined for the observations using artificial star experiments. A full description of the details of our approach and the STARPROBE software are given ...
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.