A Model Of The Galactic Tidal Interaction With The Oort Comet Cloud

1992 ◽  
pp. 13-35 ◽  
Author(s):  
John J. Matese ◽  
Patrick G. Whitman
Keyword(s):  
Tidal Interaction

scholarly journals The Post-periapsis Evolution of Galactic Center Source G1: The Second Case of a Resolved Tidal Interaction with a Supermassive Black Hole

2017 ◽  
Vol 847 (1) ◽  
pp. 80 ◽  
Author(s):  
G. Witzel ◽  
B. N. Sitarski ◽  
A. M. Ghez ◽  
M. R. Morris ◽  
A. Hees ◽  
...  
Keyword(s):  
Black Hole ◽  
Galactic Center ◽  
Tidal Interaction ◽  
Supermassive Black Hole

scholarly journals Photometric Studies of the Extreme SMC Wing

1980 ◽  
Vol 85 ◽  
pp. 353-355 ◽  
Author(s):  
William E. Kunkel
Keyword(s):  
Star Formation ◽  
Time Scales ◽  
Formation Time ◽  
Stellar Systems ◽  
Tidal Disruption ◽  
Tidal Interaction ◽  
Magellanic Stream

Among the currently interesting problems of interpreting the Magellanic Stream as an instance of tidal disruption is that of finding some demonstrable phenomenon in the makeup of the involved material that parallels the better known cases of tidal interaction, as for example NGC4038/39, where the dynamic and star-formation time scales are in agreement (Schweizer 1977). The observational problems that beset the interpretation of the Magellanic Stream are numerous (Mathewson and Schwartz 1976, Kunkel 1979, Bregman 1979), and the marked difference between the composition of the Stream (evidenced purely through HI) and the stellar systems (at least 80 percent stars) is among the outstanding dilemmas remaining. Finding some counterpart in the Magellanic scene comparable to the better recognized instances of tidal interaction may go some way towards clarifying a perplexing situation.

scholarly journals Substructure in Dwarf Galaxies

2004 ◽  
Vol 21 (4) ◽  
pp. 379-381
Author(s):  
Matthew Coleman
Keyword(s):  
Dark Matter ◽  
Star Formation ◽  
Large Scale ◽  
Stellar Population ◽  
Milky Way ◽  
Dwarf Galaxies ◽  
Tidal Interaction ◽  
Kinematic Evolution ◽  
Dark Material ◽  
Star Formation Histories

AbstractRecent years have seen a series of large-scale photometric surveys with the aim of detecting substructure in nearby dwarf galaxies. Some of these objects display a varying distribution of each stellar population, reflecting their star formation histories. Also, dwarf galaxies are dominated by dark matter, therefore luminous substructure may represent a perturbation in the underlying dark material. Substructure can also be the effect of tidal interaction, such as the disruption of the Sagittarius dSph by the Milky Way. Therefore, substructure in dwarf galaxies manifests the stellar, structural, and kinematic evolution of these objects.

scholarly journals Tidal Interaction in Binary-Black-Hole Inspiral

2001 ◽  
Vol 87 (23) ◽  
Author(s):  
Richard H. Price ◽  
John T. Whelan
Keyword(s):  
Black Hole ◽  
Tidal Interaction ◽  
Binary Black Hole

scholarly journals Star-planet tidal interaction and the limits of gyrochronology

2019 ◽  
Vol 626 ◽  
pp. A120
Author(s):  
F. Gallet ◽  
P. Delorme
Keyword(s):  
Angular Momentum ◽  
Rotation Rate ◽  
Age Determination ◽  
Rotation Period ◽  
Orbital Evolution ◽  
Tidal Interaction ◽  
Surface Rotation ◽  
Rotational Evolution ◽  
Forbidden Region ◽  
The Impact

Context. Age estimation techniques such as gyrochronology and magnetochronology cannot be applied to stars that have exchanged angular momentum with their close environments. This is especially true for a massive close-in planetary companion (with a period of a few days or less) that could have been strongly impacted by the rotational evolution of the host star, throughout the stellar evolution, through the star-planet tidal interaction. Aims. In this article, we provide the community with a reliable region in which empirical techniques such as gyrochronology can be used with confidence. Methods. We combined a stellar angular momentum evolution code with a planetary orbital evolution code to study in detail the impact of star-planet tidal interaction on the evolution of the surface rotation rate of the star. Results. We show that the interaction of a close-in massive planet with its host star can strongly modify the surface rotation rate of this latter, in most of the cases associated with a planetary engulfment. A modification of the surface rotation period of more than 90% can survive a few hundred Myr after the event and a modification of 10% can last for a few Gyr. In such cases, a gyrochronology analysis of the star would incorrectly make it appear as rejuvenated, thus preventing us from using this method with confidence. To try overcome this issue, we proposed the proof of concept of a new age determination technique that we call the tidal-chronology method, which is based on the observed pair Prot, ⋆–Porb of a given star-planet system, where Prot, ⋆ is the stellar surface rotational period and Porb the planetary orbital period. Conclusions. The gyrochronology technique can only be applied to isolated stars or star-planet systems outside a specific range of Prot, ⋆–Porb. This region tends to expand for increasing stellar and planetary mass. In that forbidden region, or if any planetary engulfment is suspected, gyrochronology should be used with extreme caution, while tidal-chronology could be considered. This technique does not provide a precise age for the system yet; however, it is already an extension of gyrochronology and could be helpful to determine a more precise range of possible ages for planetary systems composed of a star between 0.3 and 1.2 M⊙ and a planet more massive than 1 Mjup initially located at a few hundredths of au from the host star.

scholarly journals The M31/M33 tidal interaction: a hydrodynamic simulation of the extended gas distribution

2020 ◽  
Vol 493 (4) ◽  
pp. 5636-5647
Author(s):  
Thor Tepper-García ◽  
Joss Bland-Hawthorn ◽  
Di Li
Keyword(s):  
Hydrodynamic Simulation ◽  
Dynamical Mass ◽  
Tidal Interaction ◽  
The Past ◽  
Hydrodynamical Simulation ◽  
Andromeda Galaxy ◽  
History Of ◽  
Motion Measurements ◽  
Orbit Integration ◽  
Orbital Solution

ABSTRACT We revisit the orbital history of the Triangulum galaxy (M33) around the Andromeda galaxy (M31) in view of the recent Gaia Data Release 2 proper motion measurements for both Local Group galaxies. Earlier studies consider highly idealized dynamical friction, but neglect the effects of dynamical mass loss. We show the latter process to be important using mutually consistent orbit integration and N-body simulations. Following this approach, we find an orbital solution that brings these galaxies to within ∼50 kpc of each other in the past, ∼6.5 Gyr ago. We explore the implications of their interaction using an N-body/hydrodynamical simulation with a focus on the origin of two prominent features: (1) M31’s Giant Stellar Stream; and (2) the M31–M33 H i filament. We find that the tidal interaction does not produce a structure reminiscent of the stellar stream that survives up to the present day. In contrast, the M31–M33 H i filament is likely a fossil structure dating back to the time of the ancient encounter between these galaxies. Similarly, the observed outer disc warp in M33 may well be a relic of this past event. Our model suggests the presence of a tidally induced gas envelope around these galaxies, and the existence of a diffuse gas stream, the ‘Triangulum stream’, stretching for tens of kpc from M33 away from M31. We anticipate upcoming observations with the recently commissioned, Five-hundred-metre Aperture Spherical radio Telescope that will target the putative stream in its first years of operation.

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