A circumstellar dust disk around T Tauri N: Subarcsecond imaging at λ = 3 millimeters

R. L. Akeson, D. W. Koerner, E. L N Jensen

Research output: Contribution to journalArticle

52 Citations (Scopus)

Abstract

We present high-resolution imaging of the young binary T Tauri in continuum emission at λ = 3 mm. Compact dust emission with integrated flux density 50 ± 6 mJy is resolved in an aperture synthesis map at 0″5 resolution and is centered at the position of the optically visible component, T Tau N. No emission above a 3 σ level of 9 mJy is detected 0″7 south of T Tau N at the position of the infrared companion, T Tau S. We interpret the continuum detection as arising from a circumstellar disk around T Tau N, and estimate its properties by fitting a flat-disk model to visibilities at λ = 1 and 3 mm, and to the flux density at λ = 7 mm. Given the data, probability distributions are calculated for values of the free parameters, including the temperature, density, dust opacity, and disk outer radius. The radial variation in temperature and density is not narrowly constrained by the data. The most likely value of the frequency dependence of the dust opacity, β = 0.53-0.17+0.27, is consistent with that of disks around other single T Tauri stars in which grain growth is believed to have taken place. The outer radius, R = 41-14+26 AU, is smaller than the projected separation between T Tau N and T Tau S, and may indicate tidal or resonance truncation of the disk by T Tau S. The total mass estimated for the disk, log (MD/M) = -24-0.6+0.7, is similar to masses observed around many single pre-main-sequence sources and, within the uncertainties, is similar to the minimum nebular mass required to form a planetary system like our own. This observation strongly suggests that the presence of a binary companion does not rule out the possibility of formation of a sizable planetary system.

Original languageEnglish (US)
Pages (from-to)358-362
Number of pages5
JournalAstrophysical Journal
Volume505
Issue number1 PART I
DOIs
StatePublished - 1998
Externally publishedYes

Fingerprint

dust
planetary systems
opacity
frequency dependence
flux density
visibility
continuums
radii
T Tauri stars
temperature
apertures
high resolution
synthesis
estimates
approximation

Keywords

  • Circumstellar matter
  • Stars: individual (T Tauri)
  • Stars: Pre-main-sequence

ASJC Scopus subject areas

  • Space and Planetary Science

Cite this

A circumstellar dust disk around T Tauri N : Subarcsecond imaging at λ = 3 millimeters. / Akeson, R. L.; Koerner, D. W.; Jensen, E. L N.

In: Astrophysical Journal, Vol. 505, No. 1 PART I, 1998, p. 358-362.

Research output: Contribution to journalArticle

Akeson, R. L. ; Koerner, D. W. ; Jensen, E. L N. / A circumstellar dust disk around T Tauri N : Subarcsecond imaging at λ = 3 millimeters. In: Astrophysical Journal. 1998 ; Vol. 505, No. 1 PART I. pp. 358-362.
@article{c36fc30da3d94ddd8892dd09ca4181f1,
title = "A circumstellar dust disk around T Tauri N: Subarcsecond imaging at λ = 3 millimeters",
abstract = "We present high-resolution imaging of the young binary T Tauri in continuum emission at λ = 3 mm. Compact dust emission with integrated flux density 50 ± 6 mJy is resolved in an aperture synthesis map at 0″5 resolution and is centered at the position of the optically visible component, T Tau N. No emission above a 3 σ level of 9 mJy is detected 0″7 south of T Tau N at the position of the infrared companion, T Tau S. We interpret the continuum detection as arising from a circumstellar disk around T Tau N, and estimate its properties by fitting a flat-disk model to visibilities at λ = 1 and 3 mm, and to the flux density at λ = 7 mm. Given the data, probability distributions are calculated for values of the free parameters, including the temperature, density, dust opacity, and disk outer radius. The radial variation in temperature and density is not narrowly constrained by the data. The most likely value of the frequency dependence of the dust opacity, β = 0.53-0.17+0.27, is consistent with that of disks around other single T Tauri stars in which grain growth is believed to have taken place. The outer radius, R = 41-14+26 AU, is smaller than the projected separation between T Tau N and T Tau S, and may indicate tidal or resonance truncation of the disk by T Tau S. The total mass estimated for the disk, log (MD/M⊙) = -24-0.6+0.7, is similar to masses observed around many single pre-main-sequence sources and, within the uncertainties, is similar to the minimum nebular mass required to form a planetary system like our own. This observation strongly suggests that the presence of a binary companion does not rule out the possibility of formation of a sizable planetary system.",
keywords = "Circumstellar matter, Stars: individual (T Tauri), Stars: Pre-main-sequence",
author = "Akeson, {R. L.} and Koerner, {D. W.} and Jensen, {E. L N}",
year = "1998",
doi = "10.1086/306167",
language = "English (US)",
volume = "505",
pages = "358--362",
journal = "Astrophysical Journal",
issn = "0004-637X",
publisher = "IOP Publishing Ltd.",
number = "1 PART I",

}

TY - JOUR

T1 - A circumstellar dust disk around T Tauri N

T2 - Subarcsecond imaging at λ = 3 millimeters

AU - Akeson, R. L.

AU - Koerner, D. W.

AU - Jensen, E. L N

PY - 1998

Y1 - 1998

N2 - We present high-resolution imaging of the young binary T Tauri in continuum emission at λ = 3 mm. Compact dust emission with integrated flux density 50 ± 6 mJy is resolved in an aperture synthesis map at 0″5 resolution and is centered at the position of the optically visible component, T Tau N. No emission above a 3 σ level of 9 mJy is detected 0″7 south of T Tau N at the position of the infrared companion, T Tau S. We interpret the continuum detection as arising from a circumstellar disk around T Tau N, and estimate its properties by fitting a flat-disk model to visibilities at λ = 1 and 3 mm, and to the flux density at λ = 7 mm. Given the data, probability distributions are calculated for values of the free parameters, including the temperature, density, dust opacity, and disk outer radius. The radial variation in temperature and density is not narrowly constrained by the data. The most likely value of the frequency dependence of the dust opacity, β = 0.53-0.17+0.27, is consistent with that of disks around other single T Tauri stars in which grain growth is believed to have taken place. The outer radius, R = 41-14+26 AU, is smaller than the projected separation between T Tau N and T Tau S, and may indicate tidal or resonance truncation of the disk by T Tau S. The total mass estimated for the disk, log (MD/M⊙) = -24-0.6+0.7, is similar to masses observed around many single pre-main-sequence sources and, within the uncertainties, is similar to the minimum nebular mass required to form a planetary system like our own. This observation strongly suggests that the presence of a binary companion does not rule out the possibility of formation of a sizable planetary system.

AB - We present high-resolution imaging of the young binary T Tauri in continuum emission at λ = 3 mm. Compact dust emission with integrated flux density 50 ± 6 mJy is resolved in an aperture synthesis map at 0″5 resolution and is centered at the position of the optically visible component, T Tau N. No emission above a 3 σ level of 9 mJy is detected 0″7 south of T Tau N at the position of the infrared companion, T Tau S. We interpret the continuum detection as arising from a circumstellar disk around T Tau N, and estimate its properties by fitting a flat-disk model to visibilities at λ = 1 and 3 mm, and to the flux density at λ = 7 mm. Given the data, probability distributions are calculated for values of the free parameters, including the temperature, density, dust opacity, and disk outer radius. The radial variation in temperature and density is not narrowly constrained by the data. The most likely value of the frequency dependence of the dust opacity, β = 0.53-0.17+0.27, is consistent with that of disks around other single T Tauri stars in which grain growth is believed to have taken place. The outer radius, R = 41-14+26 AU, is smaller than the projected separation between T Tau N and T Tau S, and may indicate tidal or resonance truncation of the disk by T Tau S. The total mass estimated for the disk, log (MD/M⊙) = -24-0.6+0.7, is similar to masses observed around many single pre-main-sequence sources and, within the uncertainties, is similar to the minimum nebular mass required to form a planetary system like our own. This observation strongly suggests that the presence of a binary companion does not rule out the possibility of formation of a sizable planetary system.

KW - Circumstellar matter

KW - Stars: individual (T Tauri)

KW - Stars: Pre-main-sequence

UR - http://www.scopus.com/inward/record.url?scp=22444456181&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=22444456181&partnerID=8YFLogxK

U2 - 10.1086/306167

DO - 10.1086/306167

M3 - Article

AN - SCOPUS:22444456181

VL - 505

SP - 358

EP - 362

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 1 PART I

ER -