On the anomalous mass defect of strange stars in the Field
... ∆2 M magnitude is of the order of ∼ 0.15 × 1053 erg at M ∼ 0.26 M⊙ in the first branch, and ∼ 0.3 × 1053 erg at the endpoint of the third branch at M ∼ 0.9 M⊙ . A variety of behaviors can be obtained by the variation of the model parameters. Some typical examples are shown in Fig. 2. Panels (a) and ...
... ∆2 M magnitude is of the order of ∼ 0.15 × 1053 erg at M ∼ 0.26 M⊙ in the first branch, and ∼ 0.3 × 1053 erg at the endpoint of the third branch at M ∼ 0.9 M⊙ . A variety of behaviors can be obtained by the variation of the model parameters. Some typical examples are shown in Fig. 2. Panels (a) and ...
Implications for dwarf spheroidal mass content from interloper removal
... are usually measured from the velocities of the neutral hydrogen gas which is forced to be on circular orbits and tidal features would leave very obvious signatures. For one thing, escaped gas along the los would have an entirely different density to the gas inside the galaxy. Secondly, warps are rel ...
... are usually measured from the velocities of the neutral hydrogen gas which is forced to be on circular orbits and tidal features would leave very obvious signatures. For one thing, escaped gas along the los would have an entirely different density to the gas inside the galaxy. Secondly, warps are rel ...
The extended structure of the dwarf irregular galaxy Sagittarius⋆⋆⋆
... dynamics of these systems at large distances from their centres, thus probing their dark matter (DM) haloes over a wide radial range. The structure and kinematics of the neutral hydrogen provide additional and complementary information. It must be stressed that dwarf galaxies evolved in isolation sh ...
... dynamics of these systems at large distances from their centres, thus probing their dark matter (DM) haloes over a wide radial range. The structure and kinematics of the neutral hydrogen provide additional and complementary information. It must be stressed that dwarf galaxies evolved in isolation sh ...
Chapter 9 Post-main sequence evolution through helium burning
... 8 M⊙ . Both low-mass and intermediate-mass stars shed their envelopes by a strong stellar wind at the end of their evolution and their remnants are CO white dwarfs. massive stars have masses larger than Mup ≈ 8 M⊙ and ignite carbon in a non-degenerate core. Except for a small mass range (≈ 8 − 11 M⊙ ...
... 8 M⊙ . Both low-mass and intermediate-mass stars shed their envelopes by a strong stellar wind at the end of their evolution and their remnants are CO white dwarfs. massive stars have masses larger than Mup ≈ 8 M⊙ and ignite carbon in a non-degenerate core. Except for a small mass range (≈ 8 − 11 M⊙ ...
The Carina Dwarf Spheroidal Galaxy: A Goldmine for Cosmology
... – 0.0001 mag in B, V and I, respectively, based on 8795, 14 945, and 10 329 stars. The formal statistical confidence intervals on these numbers are all < 1 × 10 –4 mag, but these are certainly underestimated; we still need to think harder about how to characterise our actual systematic un certaint ...
... – 0.0001 mag in B, V and I, respectively, based on 8795, 14 945, and 10 329 stars. The formal statistical confidence intervals on these numbers are all < 1 × 10 –4 mag, but these are certainly underestimated; we still need to think harder about how to characterise our actual systematic un certaint ...
Red Supergiants, Luminous Blue Variables and Wolf
... If indeed, stars in the red supergiant stage lose more mass than currently accounted for in models then it may be that stars evolve back in the blue, ending their life either as blue supergiants, Wolf-Rayet stars or even red supergiants (if they return back to the red) but with a H-rich envelope too ...
... If indeed, stars in the red supergiant stage lose more mass than currently accounted for in models then it may be that stars evolve back in the blue, ending their life either as blue supergiants, Wolf-Rayet stars or even red supergiants (if they return back to the red) but with a H-rich envelope too ...
Roche accretion of stars close to massive black holes
... brown dwarf on to a ∼106 –107 M SMBH can produce emissions with ∼1 h period, though the mass accretion rate under adiabatic condition and pure gravitational radiation torque might be too low to produce the observed X-ray flux. In Section 2, we compute the stellar evolution in the Newtonian limit. W ...
... brown dwarf on to a ∼106 –107 M SMBH can produce emissions with ∼1 h period, though the mass accretion rate under adiabatic condition and pure gravitational radiation torque might be too low to produce the observed X-ray flux. In Section 2, we compute the stellar evolution in the Newtonian limit. W ...
Direct Imaging discovery of a second planet candidate
... and the Calar Alto observatory that reveal a directly imaged planet candidate close to the young M3 star CVSO 30. Results. The JHK-band photometry of the newly identified candidate is better than 1 σ consistent with late type giants, early T and M dwarfs as well as free-floating planets, other hypot ...
... and the Calar Alto observatory that reveal a directly imaged planet candidate close to the young M3 star CVSO 30. Results. The JHK-band photometry of the newly identified candidate is better than 1 σ consistent with late type giants, early T and M dwarfs as well as free-floating planets, other hypot ...
HMM词性标注
... moved to within 0.01 pc of a 107 Msun central BH, where the viscosity might become important, its AM per unit mass must decrease to (107 x 0.01pc/1011x104pc)~10-5 of its initial value. Gravitational interactions with other galaxies are sometimes suspected of playing a major role in fuelling AGNs. ...
... moved to within 0.01 pc of a 107 Msun central BH, where the viscosity might become important, its AM per unit mass must decrease to (107 x 0.01pc/1011x104pc)~10-5 of its initial value. Gravitational interactions with other galaxies are sometimes suspected of playing a major role in fuelling AGNs. ...
Cygnus X-1 poster (Massive Star Workshop)
... Cygnus X-1 is a luminous X-ray binary, hosting a 14.81 ± 0.98 M⊙ black hole (BH) and a 19.16 ± 1.90 M⊙ O supergiant star in a Keplerian orbit of 5.6 days (Orosz 2011). This system is a persistent X-ray source that emits in two states: low-hard or high-soft state. Although the supergiant is close to ...
... Cygnus X-1 is a luminous X-ray binary, hosting a 14.81 ± 0.98 M⊙ black hole (BH) and a 19.16 ± 1.90 M⊙ O supergiant star in a Keplerian orbit of 5.6 days (Orosz 2011). This system is a persistent X-ray source that emits in two states: low-hard or high-soft state. Although the supergiant is close to ...
Post Common Envelope Binaries from SDSS. I: 101 white dwarf
... date and time when the SDSS spectra where obtained: a significant fraction of SDSS spectra are combined from observations taken on different nights (which we will call “sub-spectra” in what follows) in which case the header keyword MJDLIST will be populated with more than one date. The headers of th ...
... date and time when the SDSS spectra where obtained: a significant fraction of SDSS spectra are combined from observations taken on different nights (which we will call “sub-spectra” in what follows) in which case the header keyword MJDLIST will be populated with more than one date. The headers of th ...
Chapter 2 Mass Transfer in Binary Systems
... medium; (2) neutron stars/black holes accreting from the wind from their massive, early type companion star in close orbits. First consider a compact star at rest in interstellar medium. We take spherical coordinate (r, ,) with origin at the center of the star. The spherical symmetry implies that ...
... medium; (2) neutron stars/black holes accreting from the wind from their massive, early type companion star in close orbits. First consider a compact star at rest in interstellar medium. We take spherical coordinate (r, ,) with origin at the center of the star. The spherical symmetry implies that ...
Magnetic susceptibility, magnetization, magnetic moment and
... photoionization modelling (MPhM) of the ionized gas using 2-D ChDSs of dwarf galaxies. We calculate emissivity maps for important nebular emission lines. Their intensities are used to derive the chemical abundance of oxygen by the so-called T e − and R23 −methods. Some disagreements are found betwee ...
... photoionization modelling (MPhM) of the ionized gas using 2-D ChDSs of dwarf galaxies. We calculate emissivity maps for important nebular emission lines. Their intensities are used to derive the chemical abundance of oxygen by the so-called T e − and R23 −methods. Some disagreements are found betwee ...
Modelling the Ultra-Faint Dwarf Galaxies and Tidal
... Before(A), while (B) Both models show high velocity dispersion after dissolution [c] C:&no density enhancement, low , C Mean vrad is patchy with gradient (B) vs. constant within object (D) gradient in vrad D ...
... Before(A), while (B) Both models show high velocity dispersion after dissolution [c] C:&no density enhancement, low , C Mean vrad is patchy with gradient (B) vs. constant within object (D) gradient in vrad D ...
Edmund C. Stoner and the discovery of the maximum mass of white
... pressure of the electrons caused by the exclusion principle. Fowler, however, did not attempt to determine the equilibrium properties of such a star which he regarded as “strictly analogous to one giant molecule in the ground state''. Apparently he was unaware that at the time, Llewellyn H. Thomas h ...
... pressure of the electrons caused by the exclusion principle. Fowler, however, did not attempt to determine the equilibrium properties of such a star which he regarded as “strictly analogous to one giant molecule in the ground state''. Apparently he was unaware that at the time, Llewellyn H. Thomas h ...
THE YELLOW SUPERGIANT PROGENITOR OF THE TYPE II
... Telescope, the Telescopio Nazionale Galileo, as well as a number of other telescopes available to the collaboration. The results of the complete follow-up campaign will be published in a forthcoming paper (M. Ergon et al. 2011, in preparation). Here we present data obtained during the first ∼50 days ...
... Telescope, the Telescopio Nazionale Galileo, as well as a number of other telescopes available to the collaboration. The results of the complete follow-up campaign will be published in a forthcoming paper (M. Ergon et al. 2011, in preparation). Here we present data obtained during the first ∼50 days ...
Evolution, Mass Loss and Variability of Low and Intermediate
... envelope giving a planetary nebula (probably bipolar, certainly asymmetric). The central remnant star will be a close binary. The observed fraction of red giants that show ellipsoidal variability, combined with models for ellipsoidal light curves can be used to estimate the fraction of planetary neb ...
... envelope giving a planetary nebula (probably bipolar, certainly asymmetric). The central remnant star will be a close binary. The observed fraction of red giants that show ellipsoidal variability, combined with models for ellipsoidal light curves can be used to estimate the fraction of planetary neb ...
Extragalactic Globular Cluster Systems
... The globular clusters that were once within the merging protogalaxies are so dense that they survive intact and will orbit freely within the Galaxy. The surviving protogalaxies may be the precursors of the old satellite galaxies, some of which host old globular clusters such as Fornax, whose morphol ...
... The globular clusters that were once within the merging protogalaxies are so dense that they survive intact and will orbit freely within the Galaxy. The surviving protogalaxies may be the precursors of the old satellite galaxies, some of which host old globular clusters such as Fornax, whose morphol ...
The observed distribution of spectroscopic binaries from the Anglo
... brown-dwarf companions while another two have eccentricities that place them in the extreme upper tail of the eccentricity distribution for binaries with periods less than 1000 d. For periods up to 12 years, the distribution of our stellar companion masses is fairly flat, mirroring that seen in othe ...
... brown-dwarf companions while another two have eccentricities that place them in the extreme upper tail of the eccentricity distribution for binaries with periods less than 1000 d. For periods up to 12 years, the distribution of our stellar companion masses is fairly flat, mirroring that seen in othe ...
Neutron stars: compact objects with relativistic
... compactness and curvature assert that relativistic gravity is indispensable for the description of neutron stars. One may thus hope to employ neutron stars for seeking deviations from general relativity or as test beds to constrain alternative or modified models of gravity [25, 27, 28]. The discover ...
... compactness and curvature assert that relativistic gravity is indispensable for the description of neutron stars. One may thus hope to employ neutron stars for seeking deviations from general relativity or as test beds to constrain alternative or modified models of gravity [25, 27, 28]. The discover ...
Presentation in PDF format.
... They are completely convective As a consequence, M dwarfs have strong magnetic fields, which drives a lot of activity, including giant spots and giant flares and bright X-ray coronae. Hydrogen-burning is by the PP chains; Brown Dwarfs (L, T, ...) are found below H-burning limit, so are not real star ...
... They are completely convective As a consequence, M dwarfs have strong magnetic fields, which drives a lot of activity, including giant spots and giant flares and bright X-ray coronae. Hydrogen-burning is by the PP chains; Brown Dwarfs (L, T, ...) are found below H-burning limit, so are not real star ...
The Sagittarius dwarf irregular galaxy: Metallicity and stellar
... content in dwarf irregular galaxies (see Mateo 1998). Because of its high gas content, low luminosity, and especially its claimed very low metallicity, SagDIG may be a clue to the origin and evolution of dwarf galaxies. Although located at the border of the Local Group it is still close enough to al ...
... content in dwarf irregular galaxies (see Mateo 1998). Because of its high gas content, low luminosity, and especially its claimed very low metallicity, SagDIG may be a clue to the origin and evolution of dwarf galaxies. Although located at the border of the Local Group it is still close enough to al ...
The Sagittarius dwarf irregular galaxy
... content in dwarf irregular galaxies (see Mateo 1998). Because of its high gas content, low luminosity, and especially its claimed very low metallicity, SagDIG may be a clue to the origin and evolution of dwarf galaxies. Although located at the border of the Local Group it is still close enough to al ...
... content in dwarf irregular galaxies (see Mateo 1998). Because of its high gas content, low luminosity, and especially its claimed very low metallicity, SagDIG may be a clue to the origin and evolution of dwarf galaxies. Although located at the border of the Local Group it is still close enough to al ...
The Sagittarius dwarf irregular galaxy: Metallicity and stellar
... content in dwarf irregular galaxies (see Mateo 1998). Because of its high gas content, low luminosity, and especially its claimed very low metallicity, SagDIG may be a clue to the origin and evolution of dwarf galaxies. Although located at the border of the Local Group it is still close enough to al ...
... content in dwarf irregular galaxies (see Mateo 1998). Because of its high gas content, low luminosity, and especially its claimed very low metallicity, SagDIG may be a clue to the origin and evolution of dwarf galaxies. Although located at the border of the Local Group it is still close enough to al ...
Interpretation of the Helix Planetary Nebula using Hydro
... by factors ≈ ×6 − 10. Because stars form from planets, the first stars must be small and early. Large ≥ 2M population III stars forming from 106 M Jeans mass gas clouds in CDM halos never happened and neither did re-ionization of the gas-epoch back to a second plasmaepoch. CDM halos never happened ...
... by factors ≈ ×6 − 10. Because stars form from planets, the first stars must be small and early. Large ≥ 2M population III stars forming from 106 M Jeans mass gas clouds in CDM halos never happened and neither did re-ionization of the gas-epoch back to a second plasmaepoch. CDM halos never happened ...