Effects of Thomson-Scattering Geometry on White-Light
... Howard and Tappin (2009), the interpretation of observations of the leading edge of a CME can be fraught with difficulties, especially at large elongations. Scattered sunlight in the inner heliosphere is not only determined by the local electron density, but also by Thomsonscattering theory. The Tho ...
... Howard and Tappin (2009), the interpretation of observations of the leading edge of a CME can be fraught with difficulties, especially at large elongations. Scattered sunlight in the inner heliosphere is not only determined by the local electron density, but also by Thomsonscattering theory. The Tho ...
- Philsci
... A number of caveats apply, and it is best to introduce them straightaway. The case study is, of course, open to alternative interpretations. It is employed as an argument in two different senses. First, the case study exemplifies the thesis that fictional assumptions play an inferential role in mod ...
... A number of caveats apply, and it is best to introduce them straightaway. The case study is, of course, open to alternative interpretations. It is employed as an argument in two different senses. First, the case study exemplifies the thesis that fictional assumptions play an inferential role in mod ...
Rotation - Indiana University Astronomy
... – Jets and winds are likely launched from the disk-magnetosphere boundary – Such winds are ubiquitous among low mass (M < 2 Msun) accreting PMS stars – Direct evidence of jets found among accreting stars as massive as M ~ 10 Msun – Energetic winds observed among more massive stars • Samples are smal ...
... – Jets and winds are likely launched from the disk-magnetosphere boundary – Such winds are ubiquitous among low mass (M < 2 Msun) accreting PMS stars – Direct evidence of jets found among accreting stars as massive as M ~ 10 Msun – Energetic winds observed among more massive stars • Samples are smal ...
On the onset of runaway stellar collisions in dense star clusters I
... They also found that collisions occur every few ten thousand years, which is roughly the time required for a collision product to reach the main-sequence. Stellar collisions also play an important role in the formation of stellar exotica in young star clusters, such as blue stragglers. If cluster pr ...
... They also found that collisions occur every few ten thousand years, which is roughly the time required for a collision product to reach the main-sequence. Stellar collisions also play an important role in the formation of stellar exotica in young star clusters, such as blue stragglers. If cluster pr ...
Astronomy Astrophysics − Orbital phase-resolved spectroscopy of 4U 1538
... by 4, 134-181 channels by 8, and 182-1199 channels by 12, so that all the spectral bins were Gaussian distributed. We tested both phenomenological and physical models commonly applied to accreting X-ray pulsars. Comptonisation models attempt to provide a better physical description of the underlying ...
... by 4, 134-181 channels by 8, and 182-1199 channels by 12, so that all the spectral bins were Gaussian distributed. We tested both phenomenological and physical models commonly applied to accreting X-ray pulsars. Comptonisation models attempt to provide a better physical description of the underlying ...
Period Changes of Delta Scuti Stars and Stellar Evolution
... D’Antona & Mazzitelli (1994) and our ZAMS models. Therefore we can conclude that both series of the computations are consistent with each other. For MS and post-MS models we performed a linear nonadiabatic analysis of low–degree oscillations (ℓ ≤ 2) using the code developed by W. Dziembowski (for a ...
... D’Antona & Mazzitelli (1994) and our ZAMS models. Therefore we can conclude that both series of the computations are consistent with each other. For MS and post-MS models we performed a linear nonadiabatic analysis of low–degree oscillations (ℓ ≤ 2) using the code developed by W. Dziembowski (for a ...
a comparison of methods for determining the molecular
... plot perfect agreement would appear as a function of constant value unity, while complete disagreement would be a function of constant value zero. The figure indicates that the agreement is extremely good for all UV field strengths at metallicities Z 10−2 . In all of these cases the disagreement ...
... plot perfect agreement would appear as a function of constant value unity, while complete disagreement would be a function of constant value zero. The figure indicates that the agreement is extremely good for all UV field strengths at metallicities Z 10−2 . In all of these cases the disagreement ...
The European Large Area ISO Survey – IV. The preliminary 90
... with bolometric luminosities calculated at 90 mm assuming constant n Ln (for ease of conversion to other luminosity scales). Our method for calculating the luminosity function in the face of this complicated selection function is dealt with in the appendix. Note that our method relies on the underly ...
... with bolometric luminosities calculated at 90 mm assuming constant n Ln (for ease of conversion to other luminosity scales). Our method for calculating the luminosity function in the face of this complicated selection function is dealt with in the appendix. Note that our method relies on the underly ...
The density of very massive evolved galaxies to z≃ 1.7
... bound to the integration has been derived in two independent ways. The first one lies in deriving the lowest luminosity that our galaxies would have at z = 0. This has been obtained by assuming a pure passive evolution from z spec to z = 0. The luminosities thus obtained are reported in Table 1 and ...
... bound to the integration has been derived in two independent ways. The first one lies in deriving the lowest luminosity that our galaxies would have at z = 0. This has been obtained by assuming a pure passive evolution from z spec to z = 0. The luminosities thus obtained are reported in Table 1 and ...
On the evolution and fate of supermassive stars
... As noted by Vink et al. (2001), while the metal lines are responsible for driving the wind, hydrogen and helium lines are sparsely populated in the spectral range where early-type stars emit most of their energy. This provides some justification for using the same mass-loss recipe for hydrogen-rich ...
... As noted by Vink et al. (2001), while the metal lines are responsible for driving the wind, hydrogen and helium lines are sparsely populated in the spectral range where early-type stars emit most of their energy. This provides some justification for using the same mass-loss recipe for hydrogen-rich ...
