The birth rate of subluminous and overluminous type Ia supernovae
... The study of Chen & Li (2009) is based on a WD + MS system and their results were summarized in an orbital period-secondary mass (log Pi , M2i ) plane. According to the situation of the primary in a primordial system at the onset of the first Roche lobe overflow (RLOF), there are three evolutionary ...
... The study of Chen & Li (2009) is based on a WD + MS system and their results were summarized in an orbital period-secondary mass (log Pi , M2i ) plane. According to the situation of the primary in a primordial system at the onset of the first Roche lobe overflow (RLOF), there are three evolutionary ...
Crash Galaxies
... in two pieces, each one continuing on its own merry way after the accident, bruised and beaten, but otherwise intact. The footballer and dancer metaphors break down, as they (believe it or not) never pass right through each other. When the velocities and sizes of two galaxies are such that they coa ...
... in two pieces, each one continuing on its own merry way after the accident, bruised and beaten, but otherwise intact. The footballer and dancer metaphors break down, as they (believe it or not) never pass right through each other. When the velocities and sizes of two galaxies are such that they coa ...
Binary and Millisecond Pulsars | SpringerLink
... then this pulsar could be a very useful probe of the equation of state of super dense matter. While the hunt for more rapidly rotating pulsars and even “sub-millisecond pulsars” continues, and most neutron star equations of state allow higher spin rates than 716 Hz, it has been suggested [38] that t ...
... then this pulsar could be a very useful probe of the equation of state of super dense matter. While the hunt for more rapidly rotating pulsars and even “sub-millisecond pulsars” continues, and most neutron star equations of state allow higher spin rates than 716 Hz, it has been suggested [38] that t ...
POLYTROPES - Princeton
... of a planet like Earth. The case n = 5 is also special, as the radius of this ”star” is infinite. It is possible to show that all polytropes with n > 5 have infinite radii. This means that only solutions with n < 5 have a surface. The two cases most interesting for real stars have n = 1.5 and n = 3, ...
... of a planet like Earth. The case n = 5 is also special, as the radius of this ”star” is infinite. It is possible to show that all polytropes with n > 5 have infinite radii. This means that only solutions with n < 5 have a surface. The two cases most interesting for real stars have n = 1.5 and n = 3, ...
- Max-Planck-Institut für Astronomie
... luminosity of the remnant. The images were then added to real sky background from GEMS. From examination of these simulated images (e.g., Fig. 1), some important points become clear. The morphological signatures of interactions between early-type galaxies are often very weak; tidal tails are broad w ...
... luminosity of the remnant. The images were then added to real sky background from GEMS. From examination of these simulated images (e.g., Fig. 1), some important points become clear. The morphological signatures of interactions between early-type galaxies are often very weak; tidal tails are broad w ...
Preferential Perpendicular Acceleration of Heavy Ionospheric Ions
... determined by the maximum of 1J v I. Note that ~ = k 1 r. Since the maxima of 1 J v 1 are separated by the zeros of J II , we call the range of ~ between the zeros as cells, numbered by p. Depending on the amplitude to (or a), the threshold criterion (15) can be satisfied over several cells. The upp ...
... determined by the maximum of 1J v I. Note that ~ = k 1 r. Since the maxima of 1 J v 1 are separated by the zeros of J II , we call the range of ~ between the zeros as cells, numbered by p. Depending on the amplitude to (or a), the threshold criterion (15) can be satisfied over several cells. The upp ...
shock structures and momentum transfer in herbig
... profile that varies spatially across the object, it is easy to become overwhelmed by the sheer volume of information. In this section we will consider how to interpret spectra of HH objects and explore what these data tell us about conditions in the flows. A. Structure of Radiative Shocks The high r ...
... profile that varies spatially across the object, it is easy to become overwhelmed by the sheer volume of information. In this section we will consider how to interpret spectra of HH objects and explore what these data tell us about conditions in the flows. A. Structure of Radiative Shocks The high r ...
Many-Minds Relativity and Quantum Mechanics
... where F is the gravitational force between two bodies of mass m1 and m2 at distance r and G is the gravitational constant (≈ 9.81 meter per second2 ), you can e.g. predict by mathematical computation the coming position of the planets in our Solar system from their current positions and velocities. ...
... where F is the gravitational force between two bodies of mass m1 and m2 at distance r and G is the gravitational constant (≈ 9.81 meter per second2 ), you can e.g. predict by mathematical computation the coming position of the planets in our Solar system from their current positions and velocities. ...
A FUSE Survey of Coronal Forbidden Lines in Late
... The study of stellar coronae historically has been relegated to the X-ray wavelengths at which high-temperature plasmas predominately radiate. Unfortunately, observational limitations, including low spectral resolution, lack of precise wavelength calibrations, small effective areas, line blending, no ...
... The study of stellar coronae historically has been relegated to the X-ray wavelengths at which high-temperature plasmas predominately radiate. Unfortunately, observational limitations, including low spectral resolution, lack of precise wavelength calibrations, small effective areas, line blending, no ...
space telescope imaging spectrograph survey of far
... Jordan et al. (2001) identified the magnetic dipole line Fe xii 1242 (and its fainter companion at 1349 Å) in a high signal-to-noise Space Telescope Imaging Spectrograph (STIS) observation of the nearby dwarf Eridani (K2 V), and found evidence of Fe xii in archival STIS echellograms of several ot ...
... Jordan et al. (2001) identified the magnetic dipole line Fe xii 1242 (and its fainter companion at 1349 Å) in a high signal-to-noise Space Telescope Imaging Spectrograph (STIS) observation of the nearby dwarf Eridani (K2 V), and found evidence of Fe xii in archival STIS echellograms of several ot ...
(Very) basic introduction to special relativity
... coordinates and one temporal coordinate. But if we ask about the distance between this moment and the homecoming event, we only need two numbers: Schoellkopf Field is half a mile from here, and it’s been four days since Friday. Can we combine this 2 numbers to get a notion of “distance” between this ...
... coordinates and one temporal coordinate. But if we ask about the distance between this moment and the homecoming event, we only need two numbers: Schoellkopf Field is half a mile from here, and it’s been four days since Friday. Can we combine this 2 numbers to get a notion of “distance” between this ...
The XXL Survey - I. Scientific motivations − XMM
... roughly 100 members. The XXL Survey covers two extragalactic areas of 25 deg2 each at a point-source sensitivity of ∼5 × 10−15 erg s−1 cm−2 in the [0.5−2] keV band (completeness limit). The survey’s main goals are to provide constraints on the dark energy equation of state from the spacetime distrib ...
... roughly 100 members. The XXL Survey covers two extragalactic areas of 25 deg2 each at a point-source sensitivity of ∼5 × 10−15 erg s−1 cm−2 in the [0.5−2] keV band (completeness limit). The survey’s main goals are to provide constraints on the dark energy equation of state from the spacetime distrib ...
Ch a n d
... An inflection in the relation between the X-ray photon index and the Eddington Ratio for nearby AGN was recently revealed independently by Constantin et al. (2009) and Gu & Cao (2009). Strikingly similar trends for X-ray binaries suggest analogous accretion physics across 6-7 orders of magnitude in ...
... An inflection in the relation between the X-ray photon index and the Eddington Ratio for nearby AGN was recently revealed independently by Constantin et al. (2009) and Gu & Cao (2009). Strikingly similar trends for X-ray binaries suggest analogous accretion physics across 6-7 orders of magnitude in ...
Binary and Millisecond Pulsars
... HMBPsare believed to originate from massive binary systems, in which the primary first forms a neutron star. As the secondary evolves, its stellar wind or Rochelobe overflow feeds matter to the neutron star. The strong magnetic field of the young neutron star funnels the accreted matter to the polar ...
... HMBPsare believed to originate from massive binary systems, in which the primary first forms a neutron star. As the secondary evolves, its stellar wind or Rochelobe overflow feeds matter to the neutron star. The strong magnetic field of the young neutron star funnels the accreted matter to the polar ...
Non-thermal emission processes in massive binaries*
... - the emission of thermal X-rays, likely produced by hydrodynamic shocks between plasma shells travelling at different velocities in the wind of isolated stars, and leading to local temperature enhancements of a few 106 K (see Feldmeier et al (1997)). The thermal nature of the X-rays produced within ...
... - the emission of thermal X-rays, likely produced by hydrodynamic shocks between plasma shells travelling at different velocities in the wind of isolated stars, and leading to local temperature enhancements of a few 106 K (see Feldmeier et al (1997)). The thermal nature of the X-rays produced within ...
Chapter 1
... ratios are higher than a cooler nebula. This is because to produce [O iii] λ4363 an electron needs to be excited to 5.3 eV, which requires more energy than for 4959/5007 which result from decay from 1 D2 level, 2.5 eV above the ground-state (see Figure 2.2). Therefore, these ratios can be used to co ...
... ratios are higher than a cooler nebula. This is because to produce [O iii] λ4363 an electron needs to be excited to 5.3 eV, which requires more energy than for 4959/5007 which result from decay from 1 D2 level, 2.5 eV above the ground-state (see Figure 2.2). Therefore, these ratios can be used to co ...
Progenitor systems of Type Ia Supernovae: mergers of white dwarfs
... Type Ia supernovae, in contrast, are found in all types of galaxies and in stellar populations of vastly different ages ( 100Myrs to a few Gyrs ) and, as far as we know, leave no compact remnant behind. Therefore they cannot originate from the death of massive stars and gravitational binding energy ...
... Type Ia supernovae, in contrast, are found in all types of galaxies and in stellar populations of vastly different ages ( 100Myrs to a few Gyrs ) and, as far as we know, leave no compact remnant behind. Therefore they cannot originate from the death of massive stars and gravitational binding energy ...
CEA
... GCN position notice (WXM) given 22 s after the beginning of the burst Raptor (LANL) observed 65 sec after burst Optical afterglow extremely faint after 2 hours GRB may have occurred on region with no surrouding gas or dust, so the shock wave had little material to smash into may support the binary ...
... GCN position notice (WXM) given 22 s after the beginning of the burst Raptor (LANL) observed 65 sec after burst Optical afterglow extremely faint after 2 hours GRB may have occurred on region with no surrouding gas or dust, so the shock wave had little material to smash into may support the binary ...
The Lagoon Nebula and its Vicinity
... can be seen in maps of CO 1–0 (Lada et al. 1976) and far-IR continuum emission (Lightfoot et al. 1984), both with resolutions of 1′ –2′ . Lada et al. found 3 bright spots, BS 1–3: The most prominent (BS 1) corresponds to the inner core of the H II region, centred on the Hourglass (clump HG and surro ...
... can be seen in maps of CO 1–0 (Lada et al. 1976) and far-IR continuum emission (Lightfoot et al. 1984), both with resolutions of 1′ –2′ . Lada et al. found 3 bright spots, BS 1–3: The most prominent (BS 1) corresponds to the inner core of the H II region, centred on the Hourglass (clump HG and surro ...