The evolution of circumstellar disks in ophiuchus binaries

Jennifer Patience, R. L. Akeson, E. L N Jensen

Research output: Contribution to journalArticle

19 Citations (Scopus)

Abstract

Four Ophiuchus binaries, two Class I systems and two Class II systems, with separations of ~450-1100 AU, were observed with the Owens Valley Radio Observatory (OVRO) millimeter interferometer. In each system, the 3 mm continuum maps show dust emission at the location of the primary star, but no emission at the position of the secondary. This result is different from observations of less evolved Class 0 binaries, in which dust emission is detected from both sources. The nondetection of secondary disks is, however, similar to the dust distribution seen in wide Class II Taurus binaries. The combined OVRO results from the Ophiuchus and Taurus binaries suggest that secondary disk masses are significantly lower than primary disk masses by the Class II stage, with initial evidence that massive secondary disks are reduced by the Class I stage. Although some of the secondaries retain hot inner disk material, the early dissipation of massive outer disks may negatively impact planet formation around secondary stars. Masses for the circumprimary disks are within the range of masses measured for disks around single T Tauri stars and, in some cases, larger than the minimum mass solar nebula. More massive primary disks are predicted by several formation models and are broadly consistent with the observations. Combining the 3 mm data with previous 1.3 mm observations, the dust opacity power-law index for each primary disk is estimated. The opacity index values are all less than the scaling for interstellar dust, possibly indicating grain growth within the circumprimary disks.

Original languageEnglish (US)
Pages (from-to)616-629
Number of pages14
JournalAstrophysical Journal
Volume677
Issue number1
DOIs
StatePublished - Apr 10 2008
Externally publishedYes

Fingerprint

dust
observatory
radio
valley
interferometer
opacity
dissipation
power law
valleys
planet
observatories
stars
solar nebula
T Tauri stars
planets
interferometers
continuums
scaling
index

Keywords

  • Planetary systems: formation
  • Stars: pre-main-sequence

ASJC Scopus subject areas

  • Space and Planetary Science

Cite this

The evolution of circumstellar disks in ophiuchus binaries. / Patience, Jennifer; Akeson, R. L.; Jensen, E. L N.

In: Astrophysical Journal, Vol. 677, No. 1, 10.04.2008, p. 616-629.

Research output: Contribution to journalArticle

Patience, Jennifer ; Akeson, R. L. ; Jensen, E. L N. / The evolution of circumstellar disks in ophiuchus binaries. In: Astrophysical Journal. 2008 ; Vol. 677, No. 1. pp. 616-629.
@article{37e382a538e848b6a07ea65c46a12d02,
title = "The evolution of circumstellar disks in ophiuchus binaries",
abstract = "Four Ophiuchus binaries, two Class I systems and two Class II systems, with separations of ~450-1100 AU, were observed with the Owens Valley Radio Observatory (OVRO) millimeter interferometer. In each system, the 3 mm continuum maps show dust emission at the location of the primary star, but no emission at the position of the secondary. This result is different from observations of less evolved Class 0 binaries, in which dust emission is detected from both sources. The nondetection of secondary disks is, however, similar to the dust distribution seen in wide Class II Taurus binaries. The combined OVRO results from the Ophiuchus and Taurus binaries suggest that secondary disk masses are significantly lower than primary disk masses by the Class II stage, with initial evidence that massive secondary disks are reduced by the Class I stage. Although some of the secondaries retain hot inner disk material, the early dissipation of massive outer disks may negatively impact planet formation around secondary stars. Masses for the circumprimary disks are within the range of masses measured for disks around single T Tauri stars and, in some cases, larger than the minimum mass solar nebula. More massive primary disks are predicted by several formation models and are broadly consistent with the observations. Combining the 3 mm data with previous 1.3 mm observations, the dust opacity power-law index for each primary disk is estimated. The opacity index values are all less than the scaling for interstellar dust, possibly indicating grain growth within the circumprimary disks.",
keywords = "Planetary systems: formation, Stars: pre-main-sequence",
author = "Jennifer Patience and Akeson, {R. L.} and Jensen, {E. L N}",
year = "2008",
month = "4",
day = "10",
doi = "10.1086/526394",
language = "English (US)",
volume = "677",
pages = "616--629",
journal = "Astrophysical Journal",
issn = "0004-637X",
publisher = "IOP Publishing Ltd.",
number = "1",

}

TY - JOUR

T1 - The evolution of circumstellar disks in ophiuchus binaries

AU - Patience, Jennifer

AU - Akeson, R. L.

AU - Jensen, E. L N

PY - 2008/4/10

Y1 - 2008/4/10

N2 - Four Ophiuchus binaries, two Class I systems and two Class II systems, with separations of ~450-1100 AU, were observed with the Owens Valley Radio Observatory (OVRO) millimeter interferometer. In each system, the 3 mm continuum maps show dust emission at the location of the primary star, but no emission at the position of the secondary. This result is different from observations of less evolved Class 0 binaries, in which dust emission is detected from both sources. The nondetection of secondary disks is, however, similar to the dust distribution seen in wide Class II Taurus binaries. The combined OVRO results from the Ophiuchus and Taurus binaries suggest that secondary disk masses are significantly lower than primary disk masses by the Class II stage, with initial evidence that massive secondary disks are reduced by the Class I stage. Although some of the secondaries retain hot inner disk material, the early dissipation of massive outer disks may negatively impact planet formation around secondary stars. Masses for the circumprimary disks are within the range of masses measured for disks around single T Tauri stars and, in some cases, larger than the minimum mass solar nebula. More massive primary disks are predicted by several formation models and are broadly consistent with the observations. Combining the 3 mm data with previous 1.3 mm observations, the dust opacity power-law index for each primary disk is estimated. The opacity index values are all less than the scaling for interstellar dust, possibly indicating grain growth within the circumprimary disks.

AB - Four Ophiuchus binaries, two Class I systems and two Class II systems, with separations of ~450-1100 AU, were observed with the Owens Valley Radio Observatory (OVRO) millimeter interferometer. In each system, the 3 mm continuum maps show dust emission at the location of the primary star, but no emission at the position of the secondary. This result is different from observations of less evolved Class 0 binaries, in which dust emission is detected from both sources. The nondetection of secondary disks is, however, similar to the dust distribution seen in wide Class II Taurus binaries. The combined OVRO results from the Ophiuchus and Taurus binaries suggest that secondary disk masses are significantly lower than primary disk masses by the Class II stage, with initial evidence that massive secondary disks are reduced by the Class I stage. Although some of the secondaries retain hot inner disk material, the early dissipation of massive outer disks may negatively impact planet formation around secondary stars. Masses for the circumprimary disks are within the range of masses measured for disks around single T Tauri stars and, in some cases, larger than the minimum mass solar nebula. More massive primary disks are predicted by several formation models and are broadly consistent with the observations. Combining the 3 mm data with previous 1.3 mm observations, the dust opacity power-law index for each primary disk is estimated. The opacity index values are all less than the scaling for interstellar dust, possibly indicating grain growth within the circumprimary disks.

KW - Planetary systems: formation

KW - Stars: pre-main-sequence

UR - http://www.scopus.com/inward/record.url?scp=42549105078&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=42549105078&partnerID=8YFLogxK

U2 - 10.1086/526394

DO - 10.1086/526394

M3 - Article

AN - SCOPUS:42549105078

VL - 677

SP - 616

EP - 629

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 1

ER -