LIDT-DD: A new self-consistent debris disc model that includes radiation pressure and couples dynamical and collisional evolution

AbstractThe first attempt at developing a fully self-consistent code coupling dynamics and collisions to study debris discs (Kral et al. 2013) is presented. So far, these two crucial mechanisms were studied separately, with N-body and statistical collisional codes respectively, because of stringent computational constraints.We present a new model named LIDT-DD which is able to follow over long timescales the coupled evolution of dynamics (including radiation forces) and collisions in a self-consistent way.

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The domain of radiatively driven mass loss in the H-R diagram

Symposium - International Astronomical Union ◽

10.1017/s0074180900013516 ◽

1979 ◽

Vol 83 ◽

pp. 235-240 ◽

Cited By ~ 1

Author(s):

David C. Abbott

Keyword(s):

Steady State ◽

Mass Loss ◽

Radiation Pressure ◽

Effective Temperature ◽

Stellar Wind ◽

Radiation Force ◽

Theoretical Uncertainty ◽

Line Radiation ◽

Consistent Model ◽

Self Consistent

Previous work by Castor, Abbott, and Klein (1975) presented a self-consistent model of a steady-state stellar wind. They also showed qualitatively that for O stars at least a static atmosphere could not exist. This paper extends that result by calculating in detail the minimum luminosity as a function of effective temperature required for the line radiation force to exceed gravity. Within the observational and theoretical uncertainty there is a one-to-one correspondence between a star's calculated ability to self-initiate a stellar wind by radiation pressure alone and the observed presence of outflowing material in the UV resonance lines.

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Metastable Helium Absorptions with 3D Hydrodynamics and Self-consistent Photochemistry. II. WASP-107b, Stellar Wind, Radiation Pressure, and Shear Instability

The Astrophysical Journal ◽

10.3847/1538-4357/abf1ed ◽

2021 ◽

Vol 914 (2) ◽

pp. 99

Author(s):

Lile Wang ◽

Fei Dai

Keyword(s):

Radiation Pressure ◽

Stellar Wind ◽

Shear Instability ◽

Metastable Helium ◽

Self Consistent

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The wind of P Cygni

International Astronomical Union Colloquium ◽

10.1017/s025292110000453x ◽

1989 ◽

Vol 113 ◽

pp. 259-260

Author(s):

J. Puls ◽

A.W.A. Pauldrach ◽

R.P. Kudritzki

Keyword(s):

Energy Distribution ◽

Mass Loss ◽

Radiation Pressure ◽

Loss Rate ◽

Mass Loss Rate ◽

Terminal Velocity ◽

Scaling Relations ◽

Self Consistent ◽

Line Pressure ◽

Eddington Limit

The stationary features of the wind of P Cygni are considerably different from those of ‘normal’ supergiant winds with comparable luminosity. In contrast to such winds, which are generally accepted to be driven by radiation pressure, P Cygni’s mass-loss rate is higher by a factor of 5, the terminal velocity is higher by a factor of 10, and the velocity law itself is much flatter than would be expected from a first glance at glance at typical scaling relations. However, these relations depend crucially and non-linearly on the star’s distance from the Eddington limit, which for P Cyg is very small (see below). Here we investigate whether the acceleration mechanism of P Cygni’s wind can also be explained by line pressure and to what extent self-consistent wind models represent the observed quantities (especially the IR energy distribution).

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A detailed self-consistent vertical Milky Way disc model

EPJ Web of Conferences ◽

10.1051/epjconf/20121910007 ◽

2012 ◽

Vol 19 ◽

pp. 10007

Author(s):

A. Just ◽

O. Golubov ◽

S. Gao

Keyword(s):

Milky Way ◽

Disc Model ◽

Self Consistent

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Simulation of 10830 Å absorption with a 3D hydrodynamic model reveals the solar He abundance in upper atmosphere of WASP-107b

Monthly Notices of the Royal Astronomical Society Letters ◽

10.1093/mnrasl/slab015 ◽

2021 ◽

Author(s):

M L Khodachenko ◽

I F Shaikhislamov ◽

L Fossati ◽

H Lammer ◽

M S Rumenskikh ◽

...

Keyword(s):

Metastable State ◽

Radiation Pressure ◽

Hydrodynamic Model ◽

Planetary System ◽

Fluid Model ◽

Upper Atmosphere ◽

Helium Abundance ◽

Velocity Range ◽

Impact Processes ◽

Self Consistent

Abstract Transmission spectroscopy of WASP-107b revealed 7–8 per cent absorption at the position of metastable HeI triplet at 10830 Å in the velocity range of [-20; 10] km/s. This absorption is stronger than that measured in other exoplanets. With a dedicated 3D self-consistent hydrodynamic multi-fluid model we simulated the expanding upper atmosphere of WASP-107b and reproduced within the observations accuracy the measured HeI absorption profiles, constraining the stellar XUV flux to (6–10) erg cm−2 s−1 at 1 a.u., and the upper atmosphere helium abundance He/H to 0.075–0.15. The radiation pressure acting on the metastable HeI atoms was shown to be an important factor influencing the absorption profiles. Its effect is counterbalanced by the collisional depopulation of the HeI metastable state. Altogether, the observed HeI absorption in WASP-107b can be interpreted with the expected reasonable parameters of the stellar-planetary system and appropriate account of the electron and atom impact processes.

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The evolution of the Kuiper belt during the formation of the outer planets

International Astronomical Union Colloquium ◽

10.1017/s0252921100031213 ◽

1999 ◽

Vol 173 ◽

pp. 37-44

Author(s):

M.D. Melita ◽

A. Brunini

Keyword(s):

Kuiper Belt ◽

Outer Planets ◽

Self Consistent ◽

Planetary Bodies ◽

Mass Depletion

AbstractA self-consistent study of the formation of planetary bodies beyond the orbit of Saturn and the evolution of Kuiper disks is carried out by means of an N-body code where accretion and gravitational encounters are considered. This investigation is focused on the aggregation of massive bodies in the outer planetary region and on the consequences of such process in the corresponding cometary belt. We study the link between the bombardment of massive bodies and mass depletion and eccentricity excitation.

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