On the origin of stars with and without planets
... either on the evolutionary stage of the star or on its age3 . In Fig. 1 we plot the T c slope against the stellar age. The plot and Table 1 clearly show that the correlation with age is quite significant and confirms the result obtained for the surface gravity: old stars are more depleted in refract ...
... either on the evolutionary stage of the star or on its age3 . In Fig. 1 we plot the T c slope against the stellar age. The plot and Table 1 clearly show that the correlation with age is quite significant and confirms the result obtained for the surface gravity: old stars are more depleted in refract ...
B Non-Conservation, Cold Dark Matter and Subpreon Model § 1
... Why does Nature choose an integer ZI2 at the pre on level? It seems almost impossible to answer this quention, if we stop at the preon model. These facts show the incompleteness of the pre on level physics. We attempt to solve these problems by stepping into a subpreon level and making fundamental m ...
... Why does Nature choose an integer ZI2 at the pre on level? It seems almost impossible to answer this quention, if we stop at the preon model. These facts show the incompleteness of the pre on level physics. We attempt to solve these problems by stepping into a subpreon level and making fundamental m ...
Chapter 14- Solar System
... Components of the Solar System Since Galileo's time, our knowledge of the solar system has increased dramatically. Galileo knew the same planets that the ancient Greeks had known-Mercury, Venus, Earth, Mars, Jupiter, and Saturn. Since Galileo's time, astronomers have discovered two more planets-Uran ...
... Components of the Solar System Since Galileo's time, our knowledge of the solar system has increased dramatically. Galileo knew the same planets that the ancient Greeks had known-Mercury, Venus, Earth, Mars, Jupiter, and Saturn. Since Galileo's time, astronomers have discovered two more planets-Uran ...
BDW Lesson 1g - Ohio Academic Standards
... 2) Was there a Planet X [14] [15] between Mars and Jupiter as predicted by the Titus Bode law [Possible, this would fit law]. The Asteroid belts now inhabit this region of the Solar System. What effects might Asteroid collision with Earth cause to the Earth’s Poles? [If large enough and at proper im ...
... 2) Was there a Planet X [14] [15] between Mars and Jupiter as predicted by the Titus Bode law [Possible, this would fit law]. The Asteroid belts now inhabit this region of the Solar System. What effects might Asteroid collision with Earth cause to the Earth’s Poles? [If large enough and at proper im ...
Abundance Anomalies In Tidal Disruption Events
... from Solar (n(He)/n(H) ≃ 0.09 for X = 0.70, Y = 0.28 and Z = 0.02). Third, they argue that the CLOUDY models used by Guillochon et al. (2014) and Gaskell & Rojas Lobos (2014) assume thermal line widths (∼ 10 km/s), far smaller than the observed line widths (> 103 km/s). Hence, for the same physical ...
... from Solar (n(He)/n(H) ≃ 0.09 for X = 0.70, Y = 0.28 and Z = 0.02). Third, they argue that the CLOUDY models used by Guillochon et al. (2014) and Gaskell & Rojas Lobos (2014) assume thermal line widths (∼ 10 km/s), far smaller than the observed line widths (> 103 km/s). Hence, for the same physical ...
How To Find Newborn Black Holes Kazumi Kashiyama (UCB)
... evaluated the strength of the shock that reached the hydrogen envelope. Using the full neutrino loss model, we found in every case tested for RSG15 and in 3 of 6 tested for RSG25 that the shock produced was larger than 1×1047 ergs, the approximate binding energy of the envelope (see Table 3). We can ...
... evaluated the strength of the shock that reached the hydrogen envelope. Using the full neutrino loss model, we found in every case tested for RSG15 and in 3 of 6 tested for RSG25 that the shock produced was larger than 1×1047 ergs, the approximate binding energy of the envelope (see Table 3). We can ...
Hydrodynamic simulations with a radiative surface Atefeh Barekat
... we cannot observe the interior of the Sun directly, there is an advanced technique named helioseismology that gives insight about some properties of the interior of the Sun. In this technique oscillatory acoustic waves are used to gain information such as temperature and velocities as the differenti ...
... we cannot observe the interior of the Sun directly, there is an advanced technique named helioseismology that gives insight about some properties of the interior of the Sun. In this technique oscillatory acoustic waves are used to gain information such as temperature and velocities as the differenti ...
Дубовиченко С
... However, the results of the phase shift analysis usually existing only in a restricted energy range, does not allow us to reconstruct unambiguously the interaction potential. Therefore, the requirement based on the reproduction of the bound energy of the nucleus in the corresponding cluster channel ...
... However, the results of the phase shift analysis usually existing only in a restricted energy range, does not allow us to reconstruct unambiguously the interaction potential. Therefore, the requirement based on the reproduction of the bound energy of the nucleus in the corresponding cluster channel ...
Kinetic equilibrium of iron in the atmospheres of cool stars
... ing mostly on surface gravity). Therefore our choice of metalpoor reference stars has led to four representatives: HD 103095 (≡ Gmb 1830) as a cool main sequence star, HD 19445 as a typical subdwarf, HD 84937 as a turnoff star and HD 140283 as a moderately cool subgiant. The last two of these referen ...
... ing mostly on surface gravity). Therefore our choice of metalpoor reference stars has led to four representatives: HD 103095 (≡ Gmb 1830) as a cool main sequence star, HD 19445 as a typical subdwarf, HD 84937 as a turnoff star and HD 140283 as a moderately cool subgiant. The last two of these referen ...
400 Years of Stellar Rotation
... As usual more information does not necessarily mean more answers, but rather more questions! For many of the stars studied with other techniques, the physical characteristics can also be derived by using asteroseismology. In contrast to main sequence stars, these data show that in evolved stars, the ...
... As usual more information does not necessarily mean more answers, but rather more questions! For many of the stars studied with other techniques, the physical characteristics can also be derived by using asteroseismology. In contrast to main sequence stars, these data show that in evolved stars, the ...
Slide 1
... • When enough material has accreted, fusion can reignite very suddenly, burning off the new material. • Material keeps being transferred to the white dwarf, and the process repeats, as illustrated ...
... • When enough material has accreted, fusion can reignite very suddenly, burning off the new material. • Material keeps being transferred to the white dwarf, and the process repeats, as illustrated ...
This is the Title - Astronomy at Swarthmore College
... surface, the metals are blown into the interstellar medium, along with the surface hydrogen and helium, by the star’s massive wind. IRC+10216, also known as CW Leo, is the most well-known example of a carbon-rich AGB star due to its proximity, about 200 pc from Earth. It is not a high mass star and ...
... surface, the metals are blown into the interstellar medium, along with the surface hydrogen and helium, by the star’s massive wind. IRC+10216, also known as CW Leo, is the most well-known example of a carbon-rich AGB star due to its proximity, about 200 pc from Earth. It is not a high mass star and ...
A minimum column density of 1gcm(
... effective adiabatic index c < 1.4 throughout its volume. As even c < 1.1–1.2 is sufficient to suppress fragmentation5, equation (1) implicitly defines a critical light-to-mass ratio ghalt above which fragmentation will halt in a cloud with a given S, d and Tb. We describe our procedure for solving t ...
... effective adiabatic index c < 1.4 throughout its volume. As even c < 1.1–1.2 is sufficient to suppress fragmentation5, equation (1) implicitly defines a critical light-to-mass ratio ghalt above which fragmentation will halt in a cloud with a given S, d and Tb. We describe our procedure for solving t ...
Excitation of Solar-like Oscillations: From PMS to MS Stellar Models
... We consider a set of 3D simulations of solar-like oscillating stars. We compute internal structure of 1D stellar models and associated eigenfunctions consistent with the 3D simulations. We then compute, on the basis of the current theoretical model of stochastic excitation, the rates at which energy ...
... We consider a set of 3D simulations of solar-like oscillating stars. We compute internal structure of 1D stellar models and associated eigenfunctions consistent with the 3D simulations. We then compute, on the basis of the current theoretical model of stochastic excitation, the rates at which energy ...