Neon and oxygen in low activity stars: towards a coronal unification
... to additionally increase jointly within allowed errors would provide a sufficient opacity increase. Several objections to this solution were raised, especially from solar observers. A reassessment of solar coronal data from the Solar Maximum Mission led to an upper limit of Ne/O = 0.18 ± 0.04 for acti ...
... to additionally increase jointly within allowed errors would provide a sufficient opacity increase. Several objections to this solution were raised, especially from solar observers. A reassessment of solar coronal data from the Solar Maximum Mission led to an upper limit of Ne/O = 0.18 ± 0.04 for acti ...
The ultracompact nature of the black hole candidate X
... is a transitional millisecond pulsar. Considering the measured orbital period (with other evidence of a white dwarf donor), and the lack of transitional millisecond pulsar features in the X-ray light curve, we suggest that this could be the first ultracompact black hole X-ray binary identified in ou ...
... is a transitional millisecond pulsar. Considering the measured orbital period (with other evidence of a white dwarf donor), and the lack of transitional millisecond pulsar features in the X-ray light curve, we suggest that this could be the first ultracompact black hole X-ray binary identified in ou ...
NGC 3801 caught in the act: A post-merger starforming early
... HLS. Some diffuse and fainter emission is also seen in the intermediate region between spiral-wisp and the HLS. The western wisp is brighter than its eastern counterpart, but they extend up to similar distances (60′′ –70′′ or 14–16 kpc) from the centre of the galaxy. NUV wisps connect to an elongate ...
... HLS. Some diffuse and fainter emission is also seen in the intermediate region between spiral-wisp and the HLS. The western wisp is brighter than its eastern counterpart, but they extend up to similar distances (60′′ –70′′ or 14–16 kpc) from the centre of the galaxy. NUV wisps connect to an elongate ...
ASTRONOMY AND ASTROPHYSICS The 10–200µm spectral
... the steep ultraviolet continuum, fλ ∝ λ1.7 , may be produced by a very dusty starburst. This was later confirmed by Bonatto et al. (1998), who reproduced the ultraviolet continuum of a sample of nearby spiral galaxies by stellar population synthesis and concluded that in the case of NGC 7582 the UV ...
... the steep ultraviolet continuum, fλ ∝ λ1.7 , may be produced by a very dusty starburst. This was later confirmed by Bonatto et al. (1998), who reproduced the ultraviolet continuum of a sample of nearby spiral galaxies by stellar population synthesis and concluded that in the case of NGC 7582 the UV ...
PH607lec07
... in heavy elements, having been created before the interstellar gas had been seriously polluted with elements heavier than helium. A good view of the central bulge of our Galaxy is given by the nearinfrared picture below, which also shows the disk extending to either side. The picture was obtained us ...
... in heavy elements, having been created before the interstellar gas had been seriously polluted with elements heavier than helium. A good view of the central bulge of our Galaxy is given by the nearinfrared picture below, which also shows the disk extending to either side. The picture was obtained us ...
A STRONGLY MAGNETIZED PULSAR WITHIN THE GRASP OF THE MILKY... SUPERMASSIVE BLACK HOLE Rea ,
... might have left behind a young neutron star traveling deep into Sgr A∗ ’s gravitational potential. On 2013 April 25, a short X-ray burst was observed from the direction of the Galactic center. With a series of observations with the Chandra and the Swift satellites, we pinpoint the associated magneta ...
... might have left behind a young neutron star traveling deep into Sgr A∗ ’s gravitational potential. On 2013 April 25, a short X-ray burst was observed from the direction of the Galactic center. With a series of observations with the Chandra and the Swift satellites, we pinpoint the associated magneta ...
Spin-Driven Changes in Neutron Star Magnetic Fields
... expected in a spinning-down neutron star whenever spin-down expels enough flux from the stellar core into the equatorial regions of the lower crust. Although this sort of event should occur less than once a millenium for a Vela-like pulsar, it should happen every few decades in a 104 year old pulsar ...
... expected in a spinning-down neutron star whenever spin-down expels enough flux from the stellar core into the equatorial regions of the lower crust. Although this sort of event should occur less than once a millenium for a Vela-like pulsar, it should happen every few decades in a 104 year old pulsar ...
THE SOLAR WIND INTERACTION WITH VENUS AND MARS
... Dennerl, 2002). The observed emissions corresponds well to the sunlit part of the planets’ atmospheres in both observations, suggesting that it is fluorescence and scattering of solar X-rays that is responsible for the X-ray emissions. Also, the observed spectra are consistent with that hypothesis ( ...
... Dennerl, 2002). The observed emissions corresponds well to the sunlit part of the planets’ atmospheres in both observations, suggesting that it is fluorescence and scattering of solar X-rays that is responsible for the X-ray emissions. Also, the observed spectra are consistent with that hypothesis ( ...
Lecture 2. Thermal evolution and surface emission of - X-Ray
... Cooling of X-ray transients “Many neutron stars in close X-ray binaries are transient accretors (transients); They exhibit X-ray bursts separated by long periods (months or even years) of quiescence. It is believed that the quiescence corresponds to a lowlevel, or even halted, accretion onto the ne ...
... Cooling of X-ray transients “Many neutron stars in close X-ray binaries are transient accretors (transients); They exhibit X-ray bursts separated by long periods (months or even years) of quiescence. It is believed that the quiescence corresponds to a lowlevel, or even halted, accretion onto the ne ...
Origin and evolution of magnetars
... spin-down of the star. Our model assumes that the magnetic flux of the neutron star is distributed as a Gaussian in the logarithm about a mean value that is described by a power law M = 0 ( 9 M p )γ G cm2 (8 M ≤ Mp ≤ 45 M ), where M p is the mass of the progeni tor. We find that we can explain ...
... spin-down of the star. Our model assumes that the magnetic flux of the neutron star is distributed as a Gaussian in the logarithm about a mean value that is described by a power law M = 0 ( 9 M p )γ G cm2 (8 M ≤ Mp ≤ 45 M ), where M p is the mass of the progeni tor. We find that we can explain ...
Physics of Galaxies 2016 Exercises with solutions – Batch II
... Figure 2: The predicted temporal evolution of the Hα emission-line equivalent width EW(Hα). These models assume a Salpeter IMF and metallicity Z = 0.020. The red line represents a singleage stellar population (red line), whereas the black line is for a stellar population that continuously forms new ...
... Figure 2: The predicted temporal evolution of the Hα emission-line equivalent width EW(Hα). These models assume a Salpeter IMF and metallicity Z = 0.020. The red line represents a singleage stellar population (red line), whereas the black line is for a stellar population that continuously forms new ...
Lectures 7
... The 5 'states' are in dynamic interaction. the coldest clouds are molecular and the densest (hydrogen molecules, CO, NH3 and other molecule)s- this is where stars form . The dust is composed of 'refractory' elements and molecules mainly carbon, silicon, iron and is responsible for most of the absorp ...
... The 5 'states' are in dynamic interaction. the coldest clouds are molecular and the densest (hydrogen molecules, CO, NH3 and other molecule)s- this is where stars form . The dust is composed of 'refractory' elements and molecules mainly carbon, silicon, iron and is responsible for most of the absorp ...
Variables, Star Clusters, and Nebulae (Professor Powerpoint)
... appears redder than it actually is . This happens because short wavelength , mainly blue starlight, is scattered more by dust than longer wavelength red light. This interstellar reddening is different from reddening due to the doppler shift. Doppler shift causes all wavelengths to lengthen equally, ...
... appears redder than it actually is . This happens because short wavelength , mainly blue starlight, is scattered more by dust than longer wavelength red light. This interstellar reddening is different from reddening due to the doppler shift. Doppler shift causes all wavelengths to lengthen equally, ...
Magnetic susceptibility, magnetization, magnetic moment and
... MSSM, the portrait for dark matter production is seriously modified from the usual WIMP miracle picture. In SUSY models with radiatively-driven naturalness (radiative natural SUSY or RNS) which include a DFSZ-like solution to the strong CP and SUSY µ problems, dark matter is expected to be an admixt ...
... MSSM, the portrait for dark matter production is seriously modified from the usual WIMP miracle picture. In SUSY models with radiatively-driven naturalness (radiative natural SUSY or RNS) which include a DFSZ-like solution to the strong CP and SUSY µ problems, dark matter is expected to be an admixt ...
Galaxies 1) What are galaxies? 2) The birth of galaxies 3
... Most galaxies are between 3,000 and 400,000 light years in diameter and can contain billions or trillions of stars. The Milky Way, our galaxy, is thought to be between 100,000 and 200,000 light years in diameter and contain between 100 and 400 billion stars, the most ancient of which are 13.7 billio ...
... Most galaxies are between 3,000 and 400,000 light years in diameter and can contain billions or trillions of stars. The Milky Way, our galaxy, is thought to be between 100,000 and 200,000 light years in diameter and contain between 100 and 400 billion stars, the most ancient of which are 13.7 billio ...
notes
... Most galaxies are between 3,000 and 400,000 light years in diameter and can contain billions or trillions of stars. The Milky Way, our galaxy, is thought to be between 100,000 and 200,000 light years in diameter and contain between 100 and 400 billion stars, the most ancient of which are 13.7 billio ...
... Most galaxies are between 3,000 and 400,000 light years in diameter and can contain billions or trillions of stars. The Milky Way, our galaxy, is thought to be between 100,000 and 200,000 light years in diameter and contain between 100 and 400 billion stars, the most ancient of which are 13.7 billio ...
Test#4
... 30. What observation of the Galaxy suggests it is much larger than the halo and contains a large amount of matter not in the form of stars? a) The rotation curve, b) Motions of the globular clusters c) The shape of the spiral arms, d) Infrared observations of the center of the Galaxy 31. Quasars wer ...
... 30. What observation of the Galaxy suggests it is much larger than the halo and contains a large amount of matter not in the form of stars? a) The rotation curve, b) Motions of the globular clusters c) The shape of the spiral arms, d) Infrared observations of the center of the Galaxy 31. Quasars wer ...
Nata_Feb8 - University of Alberta
... NOTE: this defines intensity only for a non-point type object. The total luminosity L of a galaxy is difficult to define precisely for several reasons: – galaxies do not have well-defined edges, and the extended regions are faint and have a low luminosity gradient. – light from a distant galaxy is r ...
... NOTE: this defines intensity only for a non-point type object. The total luminosity L of a galaxy is difficult to define precisely for several reasons: – galaxies do not have well-defined edges, and the extended regions are faint and have a low luminosity gradient. – light from a distant galaxy is r ...
Dark bursts - indico in2p3
... Millimeter observations of afterglows with JVLA, ALMA, PdB IRAM etc. allow to determine subarcsecond positions of the GRB and may help to find a robust association with its host galaxy. Dark GRBs mostly prefer the host galaxies without radio counterpart. It means that those galaxies do not have star ...
... Millimeter observations of afterglows with JVLA, ALMA, PdB IRAM etc. allow to determine subarcsecond positions of the GRB and may help to find a robust association with its host galaxy. Dark GRBs mostly prefer the host galaxies without radio counterpart. It means that those galaxies do not have star ...
ertan et al 11cesme
... For Tp = 100 K, the Lx cutoff puts an upper limit to the observable periods of AXP/SGRs. For the sources with weaker magnetic dipole fields, rin comes out of the light cylinder earlier than it does for the sources with stronger dipole fields. After this point, P remains almost constant because of d ...
... For Tp = 100 K, the Lx cutoff puts an upper limit to the observable periods of AXP/SGRs. For the sources with weaker magnetic dipole fields, rin comes out of the light cylinder earlier than it does for the sources with stronger dipole fields. After this point, P remains almost constant because of d ...
Stellar Dynamics
... of the Milky Way appear to lie in a flattened disk-like distribution. The mid-plane of this distribution is called the “supergalactic plane”, which is nearly perpendicular to the disk of the Milky Way. In Groups, the dominant species of galaxies tend to be spirals (there are Groups known to consist ...
... of the Milky Way appear to lie in a flattened disk-like distribution. The mid-plane of this distribution is called the “supergalactic plane”, which is nearly perpendicular to the disk of the Milky Way. In Groups, the dominant species of galaxies tend to be spirals (there are Groups known to consist ...
Spectral line mapping of the Milky Way
... of weaker maser components, tracing kinematics and magnetic fields over a more extended region. These observations will also uncover the whole catalog of some particularly interesting OH-emitting evolved objects, of which very few members are known so far, such as post-AGB stars undergoing collimate ...
... of weaker maser components, tracing kinematics and magnetic fields over a more extended region. These observations will also uncover the whole catalog of some particularly interesting OH-emitting evolved objects, of which very few members are known so far, such as post-AGB stars undergoing collimate ...
Neutron stars: compact objects with relativistic
... where Ṁ is the accretion rate onto the neutron star [81]. The strong magnetic field of the neutron star channels the matter to the magnetic poles where its kinetic energy is thermalized. Radiation emitted from the accretion column or the hot spot on the surface is modulated at the rotation rate. In ...
... where Ṁ is the accretion rate onto the neutron star [81]. The strong magnetic field of the neutron star channels the matter to the magnetic poles where its kinetic energy is thermalized. Radiation emitted from the accretion column or the hot spot on the surface is modulated at the rotation rate. In ...
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.