In search of other planetary systems

Black, David C.

doi:10.1007/bf00200797

Cited by 66 publications

(13 citation statements)

References 22 publications

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“…Nearly two decades ago, Black (1980) pointed out the evident difficulties that would be encountered in interpreting the nature of any low-mass object to be found orbiting another star, lacking detailed information on the physical state of the object. The controversy over identiÐca-tion of recently discovered LMCs amply justiÐes his prescient concern.…”

Section: Formationmentioning

confidence: 99%

On the Nature of Low‐Mass Companions to Solar‐like Stars

Heacox

1999

ApJ

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Low-mass companions (mass \70 Jupiter masses) to solar-like stars are compared statistically to stellar-mass secondaries in binaries of similar primary spectral types and orbital scales, based largely on the survey of Duquennoy & Mayor. To within the limits imposed by observational constraints, the orbital properties of these low-mass companions (LMCs) are statistically indistinguishable from those of binary systems. In both populations, orbital periods (P), semimajor axes (a), angular momenta (L ), and binding energies (U) are all distributed approximately as f (x) P x~1 for x \ P, a, L , U. In both populations, eccentricities are broadly distributed approximately as f (e) P e~0.5, with no signiÐcant correlation with other orbital elements, apart from a marked circularization of close orbits. The distribution of LMC masses is approximately a power law with index between [1 and [2 ; there is ambiguous evidence in the data for a mass spectrum bimodality about approximately 10 Jupiter masses. In both populations the joint distributions of mass with all orbital properties are largely scattergrams, with no statistically signiÐcant correlations. The overall statistical properties of LMCs are suggestive of a common formation mechanism with binary star systems. The similar form of the distributions of all orbital dynamic quantities in both populations may result from postformation dissipative orbital decay.

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Section: Formationmentioning

confidence: 99%

On the Nature of Low‐Mass Companions to Solar‐like Stars

Heacox

1999

ApJ

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“…There is an additional orbital signature that could be useful as a criterion to determine whether a companion is a planet (Black 1980). This arises again from the formation mode, namely, more than one companion is formed and the resultant orbital architecture is characteristic of that process, and that architecture differs from that of a multiple star system.…”

Section: Shown Inmentioning

confidence: 99%

Possible Observational Criteria for Distinguishing Brown Dwarfs from Planets

Black

1997

The Astrophysical Journal

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The difference in formation process between binary stars and planetary systems is reflected in their composition, as well as orbital architecture, particularly in their orbital eccentricity as a function of orbital period. It is suggested here that this difference can be used as an observational criterion to distinguish between brown dwarfs and planets. Application of the orbital criterion suggests that, with three possible exceptions, all of the recently discovered substellar companions may be brown dwarfs and not planets. These criterion may be used as a guide for interpretation of the nature of substellar-mass companions to stars in the future.

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“…Astrometry from space also complements other techniques being used and proposed to detect planets (Black 1980). Some other techniques work best the smaller the planetary orbits; astrometry is preferentially sensitive to large orbits.…”

Section: Astrometry As Chosen Methodsmentioning

confidence: 97%

Astrometric Telescope Of Ten Microarcsecond Accuracy On The Space Station

et al. 1986

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We describe an Astrometric Telescope Facility (ATF) which is intended to be operated on the Space Station in the 1990's. The main purpose of the telescope will be to do long -term, highly accurate relative astrometry of nearby stars to detect gravitational perturbations by companions with masses as small as Neptune.This will require astrometry accurate to 10 microarcseconds, at least 100 times better than that currently being done at ground -based observatories, and the operation of a facility in space for many years.Because the NASA Space Station is expected to be a permanent and continuously occupied base in low earth orbit, the system described here involves an articulated telescope mount at one of the upper points of attachment on the Space Station structure.

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In search of other planetary systems

Cited by 66 publications

References 22 publications

On the Nature of Low‐Mass Companions to Solar‐like Stars

On the Nature of Low‐Mass Companions to Solar‐like Stars

Possible Observational Criteria for Distinguishing Brown Dwarfs from Planets

Astrometric Telescope Of Ten Microarcsecond Accuracy On The Space Station

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