IUE observations of Beta Pictoris - an IRAS candidate for a proto-planetary system

1985 ◽  
Vol 291 ◽  
pp. L1 ◽  
Author(s):  
Y. Kondo ◽  
F. C. Bruhweiler
Keyword(s):  
Planetary System ◽  
Beta Pictoris

scholarly journals Planetary Systems

1999 ◽  
Vol 172 ◽  
pp. 313-316
Author(s):  
Pawel Artymowicz
Keyword(s):  
Radial Velocity ◽  
Main Sequence ◽  
Direct Evidence ◽  
Planetary System ◽  
Planetary Systems ◽  
Main Sequence Stars ◽  
The Past ◽  
Exoplanetary Systems ◽  
Beta Pictoris

AbstractThe past decade brought direct evidence of the previously surmised exoplanetary systems. A variety of planetary system types exist those around pulsars, around both young and old main-sequence stars (as evidenced by planetesimal disks of the Beta Pictoris-type), and the mature giant exoplanets found in radial velocity surveys. The surprising diversity of the exoplanetary systems is addressed by several theories of their origin.

scholarly journals On the Nature of the Beta Pictoris Circumstellar Nebula

1989 ◽  
Vol 120 ◽  
pp. 221-226
Author(s):  
Francesco Paresce ◽  
Pawel Artymowicz
Keyword(s):  
Detailed Analysis ◽  
Radiation Pressure ◽  
Planetary System ◽  
Physical Characteristics ◽  
Optical Data ◽  
Beta Pictoris ◽  
Small Grains

SummaryWe summarize the observed properties and deduced physical characteristics of the Beta Pictoris circumstellar nebula obtained from a detailed analysis of existing IR and optical data. On the basis of these results, we reject the hypothesis that the observed feature is a bipolar nebula surrounding an evolved star. We claim the nebula is a flattened disk of orbiting particles making up a planetary system in its clearing out phase as small grains collide, erode, and are swept out by radiation pressure.

51. Bioastronomy - Search for Extraterrestrial Life: Bioastronomie - Recherche De La Vie Dans L’univers

1988 ◽  
Vol 20 (1) ◽  
pp. 693-701
Author(s):  
F. D. Drake ◽  
George Marx ◽  
N. D. Papagiannis ◽  
R. D. Brown ◽  
P. Connes ◽  
...  
Keyword(s):  
Planetary System ◽  
Brown Dwarf ◽  
Extraterrestrial Life ◽  
The Past ◽  
Beta Pictoris ◽  
Infra Red ◽  
Nearby Stars ◽  
Optical Wavelengths ◽  
The Many ◽  
Dust Disks

The past three years have seen not only a growth in the activities of our commission, but an extension of its activities into important areas which have heretofore motivated too little activity. Of particular interest have been the many activities directed towards elucidating the question of the abundance of extrasolar planetary systems. There have been a number of observations showing the presence of disks of dust around nearby stars, disks which fit the idea that stars are often formed with an accompanying disk of dust which may in many or perhaps all cases produce a planetary system. Infra-red evidence for dust disks exists for something like twenty stars. The disk of Beta Pictoris has even been clearly imaged at optical wavelengths, showing without a doubt that such disk structures exist. One very impressive detection of an apparent brown dwarf object has also been made; should this be confirmed by other observations, it would be clear evidence for the existence of planet-like bodies in the systems of other stars.

scholarly journals Spectral Variability of Beta Pictoris and the Search for Nearby Proto-Planetary Systems

1987 ◽  
Vol 92 ◽  
pp. 526-528
Author(s):  
F.C. Bruhweiler ◽  
Y. Kondo
Keyword(s):  
Spectral Resolution ◽  
Planetary System ◽  
Planetary Systems ◽  
High Spectral Resolution ◽  
Spectral Variability ◽  
Absorption Component ◽  
Gaseous Disk ◽  
International Ultraviolet Explorer ◽  
Beta Pictoris ◽  
Excess Absorption

Continued UV monitoring at high spectral resolution utilizing the International Ultraviolet Explorer (IUE) of the IRAS candidate proto-planetary system, Beta Pictoris (Also see Kondo and Bruhweiler 1985; and references cited therein.), has revealed two components to the circumstellar absorption. The first is a stable absorption component at or near the stellar photospheric velocity, possibly arising from gas orbiting in a gaseous disk, while the second component represents strong variable excess absorption sometimes extending up to +200 km s-1. The variability of this second component accounts for most of the spectral variability observed in Beta Pic. Variable circumstellar absorption observed in the resonance lines and UV62 and 63 multiplets of Fe II reveal an episode of mass inflow which lasted over a period of 12 to 13 months (see Fig. 1).

Mass outflow in the nearby proto-planetary system, Beta Pictoris

1991 ◽  
Vol 371 ◽  
pp. L27 ◽  
Author(s):  
Frederick C. Bruhweiler ◽  
C. A. Grady ◽  
Yoji Kondo
Keyword(s):  
Planetary System ◽  
Beta Pictoris ◽  
Mass Outflow

Annual gazetteer of planetary nomenclature, Intenationl astronomical union, working group for planetary system nomenclature

1986 ◽  
Author(s):  
Harold Masursky ◽  
Kaare Aksnes ◽  
G.E. Hunt ◽  
M.Y. Marov ◽  
P.M. Millman ◽  
...  
Keyword(s):  
Working Group ◽  
Planetary System

Drifting Through a Planetary System

2018 ◽  
Author(s):  
Karel Schrijver
Keyword(s):  
Seventeenth Century ◽  
Solar System ◽  
Virtual Worlds ◽  
Planetary System ◽  
System P ◽  
History Of ◽  
Or Team ◽  
Water Contents

This chapter describes how the first found exoplanets presented puzzles: they orbited where they should not have formed or where they could not have survived the death of their stars. The Solar System had its own puzzles to add: Mars is smaller than expected, while Venus, Earth, and Mars had more water—at least at one time—than could be understood. This chapter shows how astronomers worked through the combination of these puzzles: now we appreciate that planets can change their orbits, scatter water-bearing asteroids about, steal material from growing planets, or team up with other planets to stabilize their future. The special history of Jupiter and Saturn as a pair bringing both destruction and water to Earth emerged from the study of seventeenth-century resonant clocks, from the water contents of asteroids, and from experiments with supercomputers imposing the laws of physics on virtual worlds.

scholarly journals DESTINY: Database for the Effects of STellar encounters on dIsks and plaNetary sYstems

2019 ◽  
Vol 6 (1) ◽  
Author(s):  
Asmita Bhandare ◽  
Susanne Pfalzner
Keyword(s):  
Planetary System ◽  
Planetary Systems ◽  
Gravitational Effect ◽  
Parameter Study ◽  
Orbital Inclination ◽  
Particle Properties ◽  
Disk Size ◽  
Stellar Group ◽  
Cluster Environment ◽  
Parabolic Orbits

Abstract Most stars form as part of a stellar group. These young stars are mostly surrounded by a disk from which potentially a planetary system might form. Both, the disk and later on the planetary system, may be affected by the cluster environment due to close fly-bys. The here presented database can be used to determine the gravitational effect of such fly-bys on non-viscous disks and planetary systems. The database contains data for fly-by scenarios spanning mass ratios between the perturber and host star from 0.3 to 50.0, periastron distances from 30 au to 1000 au, orbital inclination from 0∘ to 180∘ and angle of periastron of 0∘, 45∘ and 90∘. Thus covering a wide parameter space relevant for fly-bys in stellar clusters. The data can either be downloaded to perform one’s own diagnostics like for e.g. determining disk size, disk mass, etc. after specific encounters, obtain parameter dependencies or the different particle properties can be visualized interactively. Currently the database is restricted to fly-bys on parabolic orbits, but it will be extended to hyperbolic orbits in the future. All of the data from this extensive parameter study is now publicly available as DESTINY.

scholarly journals GJ 436b and the stellar wind interaction: simulations constraints using Lyα and Hα transits

2020 ◽  
Author(s):  
Carolina Villarreal D’Angelo ◽  
Aline A Vidotto ◽  
Alejandro Esquivel ◽  
Gopal Hazra ◽  
Allison Youngblood
Keyword(s):  
Mass Loss ◽  
Stellar Wind ◽  
Planetary System ◽  
Neutral Hydrogen ◽  
Hydrogen Atmosphere ◽  
Planetary Atmosphere ◽  
Hydrodynamic Simulations ◽  
Stellar Disc ◽  
Planetary Mass ◽  
Best Fit

Abstract The GJ 436 planetary system is an extraordinary system. The Neptune-size planet that orbits the M3 dwarf revealed in the Lyα line an extended neutral hydrogen atmosphere. This material fills a comet-like tail that obscures the stellar disc for more than 10 hours after the planetary transit. Here, we carry out a series of 3D radiation hydrodynamic simulations to model the interaction of the stellar wind with the escaping planetary atmosphere. With these models, we seek to reproduce the $\sim 56\%$ absorption found in Lyα transits, simultaneously with the lack of absorption in Hα transit. Varying the stellar wind strength and the EUV stellar luminosity, we search for a set of parameters that best fit the observational data. Based on Lyα observations, we found a stellar wind velocity at the position of the planet to be around [250-460] km s−1 with a temperature of [3 − 4] × 105 K. The stellar and planetary mass loss rates are found to be 2 × 10−15 M⊙ yr−1 and ∼[6 − 10] × 109 g s−1, respectively, for a stellar EUV luminosity of [0.8 − 1.6] × 1027 erg s−1. For the parameters explored in our simulations, none of our models present any significant absorption in the Hα line in agreement with the observations.

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