1410.PDF
... of about 11MJ which can produce currents of about 20 MA within the thin conductive wires between the anode and cathode (see Fig. 1) over a time scale of about 100 ns. Usually, a few hundred wires are used to generate the Z pinch source within the primary hohlraum whose typical diameters are 2 5 cm w ...
... of about 11MJ which can produce currents of about 20 MA within the thin conductive wires between the anode and cathode (see Fig. 1) over a time scale of about 100 ns. Usually, a few hundred wires are used to generate the Z pinch source within the primary hohlraum whose typical diameters are 2 5 cm w ...
Deexcitation NSS 2004
... Is an X-Ray spectrometer to measure the composition of the upper layers of planetary surface ...
... Is an X-Ray spectrometer to measure the composition of the upper layers of planetary surface ...
The Relative Ages of M5 and Pal 4/Eridanus from their
... these form the basic building blocks of the visible matter in the Universe. ...
... these form the basic building blocks of the visible matter in the Universe. ...
Ch a n d
... The Relativistic Reflection Model Interpretation For NLS1 Soft X-Ray Lines Thomas Boller MPE Garching We have studied soft X-ray lines in Narrow-Line Seyfert 1 galaxies with XMM-Newton RGS data. Simple continuum models are ruled out, however, the relativistic reflection model by Ross & Fabian (2005 ...
... The Relativistic Reflection Model Interpretation For NLS1 Soft X-Ray Lines Thomas Boller MPE Garching We have studied soft X-ray lines in Narrow-Line Seyfert 1 galaxies with XMM-Newton RGS data. Simple continuum models are ruled out, however, the relativistic reflection model by Ross & Fabian (2005 ...
Radio and X-ray signatures of merging neutron stars
... cos a ), i.e. c is the polar angle in the frame aligned with V and rotating with the neutron star. This charge density is stationary in the frame of the neutron star while in the laboratory frame it yields an additional surface current j srot V r: The magnetic field resulting from this current i ...
... cos a ), i.e. c is the polar angle in the frame aligned with V and rotating with the neutron star. This charge density is stationary in the frame of the neutron star while in the laboratory frame it yields an additional surface current j srot V r: The magnetic field resulting from this current i ...
ASTR-1020: Astronomy II Course Lecture Notes - Faculty
... E. The Galactic Nucleus. 1. The central nuclear region of the Galaxy is completely invisible at visible wavelengths due to dust and gas obscuration. 2. However, we can see it in radio waves, since dust and gas are transparent to radio waves. The center of the galaxy is the brightest radio source in ...
... E. The Galactic Nucleus. 1. The central nuclear region of the Galaxy is completely invisible at visible wavelengths due to dust and gas obscuration. 2. However, we can see it in radio waves, since dust and gas are transparent to radio waves. The center of the galaxy is the brightest radio source in ...
The ROSAT galactic plane survey: ASTRONOMY AND
... correlation of RGPS source positions with astronomical catalogues, mostly extracted from the SIMBAD database. The historical development of astronomy has favoured galactic studies and the number of Milky Way objects held in catalogues is rather large. With the positional accuracy of the survey, up t ...
... correlation of RGPS source positions with astronomical catalogues, mostly extracted from the SIMBAD database. The historical development of astronomy has favoured galactic studies and the number of Milky Way objects held in catalogues is rather large. With the positional accuracy of the survey, up t ...
Laboratory Studies of Organic Chemistry in Space A. Ciaravella
... ● mostly gas and dust existing over a wide range of physical conditions ...
... ● mostly gas and dust existing over a wide range of physical conditions ...
Star Life Cycle
... 17. How big is a low mass star? _________________ What stages does it go through? ___________________________________________________ How big is it? ____________________________ What does it become in the end? __________________ 18. How big is a medium mass star? ________________________ What stages ...
... 17. How big is a low mass star? _________________ What stages does it go through? ___________________________________________________ How big is it? ____________________________ What does it become in the end? __________________ 18. How big is a medium mass star? ________________________ What stages ...
Stellar Winds and Supernova Remnants: Interaction with the ISM
... V-band image of IRC+10216 showing shell-like structures in the circumstellar envelope (90''x 90'') Mauron & Huggins (2010) ...
... V-band image of IRC+10216 showing shell-like structures in the circumstellar envelope (90''x 90'') Mauron & Huggins (2010) ...
Week 11 notes
... • The typical speed of galaxies within a group or cluster, as measured by the velocity dispersion, indicates the strength of the gravitational field. • The line-of-sight velocity dispersion of groups is in the range 100—500 km/s, while that of clusters is in the range ...
... • The typical speed of galaxies within a group or cluster, as measured by the velocity dispersion, indicates the strength of the gravitational field. • The line-of-sight velocity dispersion of groups is in the range 100—500 km/s, while that of clusters is in the range ...
An extended X-ray object ejected from the PSR B1259
... the same orbital cycle, the strongest variations are seen around periastron. In particular, the X-ray light curve shows two peaks corresponding to first and second passages of the pulsar through the disk (≈ 20−4 days before periastron and ≈ 10−50 days after periastron), while the hydrogen column den ...
... the same orbital cycle, the strongest variations are seen around periastron. In particular, the X-ray light curve shows two peaks corresponding to first and second passages of the pulsar through the disk (≈ 20−4 days before periastron and ≈ 10−50 days after periastron), while the hydrogen column den ...
Rotational spin-up in the 30-Myr
... shown in Fig.2, the latter cluster lacks rotational period measurements for solar-mass stars (those shown in Fig.1 are for 0.6-0.9 M stars), and has too few measurements at lower masses down to 0.3 M to allow a robust derivation of the mass-dependent rotational distribution at this age (Irwin et a ...
... shown in Fig.2, the latter cluster lacks rotational period measurements for solar-mass stars (those shown in Fig.1 are for 0.6-0.9 M stars), and has too few measurements at lower masses down to 0.3 M to allow a robust derivation of the mass-dependent rotational distribution at this age (Irwin et a ...
McConnell XGPolarimetry SSE
... angle are obtained, which provide a probe of gravity in a strong field regime and a tool to estimate the black hole parameters, and in particular its spin. Galactic Black Hole Binaries (GBHB) provide possibly the cleanest example of the use of polarimetry to test strong gravity. In these systems, wh ...
... angle are obtained, which provide a probe of gravity in a strong field regime and a tool to estimate the black hole parameters, and in particular its spin. Galactic Black Hole Binaries (GBHB) provide possibly the cleanest example of the use of polarimetry to test strong gravity. In these systems, wh ...
Stellar Magnetic Activity
... to 0.5 Mo .. The lower mass limit is the critical mass for hydrogen burning in the central cores of stars with solar abundances, while the upper limit corresponds to the spectral class M0. The radii of the red dwarfs span from 0.2R o . to about 0.6Ro . while their effective temperatures are in the r ...
... to 0.5 Mo .. The lower mass limit is the critical mass for hydrogen burning in the central cores of stars with solar abundances, while the upper limit corresponds to the spectral class M0. The radii of the red dwarfs span from 0.2R o . to about 0.6Ro . while their effective temperatures are in the r ...
Terzan 5`s Pulsars Fastest
... o The fast rotation of Ter5ad constrains its radius to be < 16 km, assuming its mass is less than 2 Msun (Fig 1). o The spin rate of Ter5ad is also an important input for models that propose gravitional radiation as a mechanism for limiting the rotation rate of neutron stars [10,11]. o The difficult ...
... o The fast rotation of Ter5ad constrains its radius to be < 16 km, assuming its mass is less than 2 Msun (Fig 1). o The spin rate of Ter5ad is also an important input for models that propose gravitional radiation as a mechanism for limiting the rotation rate of neutron stars [10,11]. o The difficult ...
Document
... Ordinary cooling isolates neutron stars of age 1 kyr—1 Myr • There is one basic phenomenological cooling concept (but many physical realizations) • Main cooling regulator: neutrino luminosity function • Warmest observed stars are low-massive; their neutrino luminosity should be < 1/30 of modified Ur ...
... Ordinary cooling isolates neutron stars of age 1 kyr—1 Myr • There is one basic phenomenological cooling concept (but many physical realizations) • Main cooling regulator: neutrino luminosity function • Warmest observed stars are low-massive; their neutrino luminosity should be < 1/30 of modified Ur ...
Evolution of Neutron Star Magnetic Fields
... The vortex-fluxoid coupling model has been developed considerably since its first suggestion, and application to various classes of neutron stars has been explored in some detail. The most comprehensive work to date is by Jahan-Miri (2000), who finds that it is possible to reproduce the long-lived l ...
... The vortex-fluxoid coupling model has been developed considerably since its first suggestion, and application to various classes of neutron stars has been explored in some detail. The most comprehensive work to date is by Jahan-Miri (2000), who finds that it is possible to reproduce the long-lived l ...
The Birth and Evolution of Brown Dwarfs
... of radio emission for spectral types cooler than M8. The decline may be shifted to cooler temperatures. • Radio emission requires magnetic fields B~5-20 G, similar to Jupiter’s ...
... of radio emission for spectral types cooler than M8. The decline may be shifted to cooler temperatures. • Radio emission requires magnetic fields B~5-20 G, similar to Jupiter’s ...
Chapter 18 - Stars - University of New Mexico
... • True nature is not yet known – but this material is most of the mass of the Universe. ...
... • True nature is not yet known – but this material is most of the mass of the Universe. ...
Active Galaxies
... Active galaxies have an energy source beyond what can be attributed to stars. The energy is believed to originate from accretion onto a supermassive blackhole. Active galaxies tend to have higher overall luminosities and very ...
... Active galaxies have an energy source beyond what can be attributed to stars. The energy is believed to originate from accretion onto a supermassive blackhole. Active galaxies tend to have higher overall luminosities and very ...
Interacting binary stars Properties of some binary stars are
... has too much angular momentum to fall directly onto the surface of the other star: Gas forms an accretion disk around the mass gaining star, through which the gas slowly spirals in before being accreted. This occurs if the accreting star does not have a strong magnetic field. ...
... has too much angular momentum to fall directly onto the surface of the other star: Gas forms an accretion disk around the mass gaining star, through which the gas slowly spirals in before being accreted. This occurs if the accreting star does not have a strong magnetic field. ...
the xmm-newton wide-field survey in the cosmos field
... 2007). The final sample comprises 135 objects. We show the distribution of their net counts in the 0.3Y10 keV band in Figure 1 and the 0.5Y10 keV flux distribution (Fig. 2) that covers a range of 1:4 ; 1015 to 1:2 ; 1013 ergs cm2 s1. From their optical spectra, we can further subdivide our sampl ...
... 2007). The final sample comprises 135 objects. We show the distribution of their net counts in the 0.3Y10 keV band in Figure 1 and the 0.5Y10 keV flux distribution (Fig. 2) that covers a range of 1:4 ; 1015 to 1:2 ; 1013 ergs cm2 s1. From their optical spectra, we can further subdivide our sampl ...
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.