M STARS in the TW HYA ASSOCIATION: STELLAR X-RAYS and DISK DISSIPATION

Costanza Argiroffi, Costanza Argiroffi, Uma Gorti, Ilaria Pascucci, David A. Principe, Joel H. Kastner, Beate Stelzer, Kristina Punzi

Risultato della ricerca: Article

11 Citazioni (Scopus)

Abstract

To investigate the potential connection between the intense X-ray emission from young low-mass stars and the lifetimes of their circumstellar planet-forming disks, we have compiled the X-ray luminosities (L X) of M stars in the ∼8 Myr old TW Hya Association (TWA) for which X-ray data are presently available. Our investigation includes analysis of archival Chandra data for the TWA binary systems TWA 8, 9, and 13. Although our study suffers from poor statistics for stars later than M3, we find a trend of decreasing with decreasing T eff for TWA M stars, wherein the earliest-type (M0-M2) stars cluster near and then decreases, and its distribution broadens, for types M4 and later. The fraction of TWA stars that display evidence for residual primordial disk material also sharply increases in this same (mid-M) spectral type regime. This apparent anticorrelation between the relative X-ray luminosities of low-mass TWA stars and the longevities of their circumstellar disks suggests that primordial disks orbiting early-type M stars in the TWA have dispersed rapidly as a consequence of their persistent large X-ray fluxes. Conversely, the disks orbiting the very lowest-mass pre-MS stars and pre-MS brown dwarfs in the Association may have survived because their X-ray luminosities and, hence, disk photoevaporation rates are very low to begin with, and then further decline relatively early in their pre-MS evolution.
Lingua originaleEnglish
pagine (da-a)3-
Numero di pagine11
RivistaTHE ASTRONOMICAL JOURNAL
Volume152
Stato di pubblicazionePublished - 2016

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M stars
x rays
stars
luminosity
late stars
star clusters
planet
planets
statistics
trends
life (durability)
distribution
analysis
rate
material
young
trend

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cita questo

Argiroffi, C., Argiroffi, C., Gorti, U., Pascucci, I., Principe, D. A., Kastner, J. H., ... Punzi, K. (2016). M STARS in the TW HYA ASSOCIATION: STELLAR X-RAYS and DISK DISSIPATION. THE ASTRONOMICAL JOURNAL, 152, 3-.

M STARS in the TW HYA ASSOCIATION: STELLAR X-RAYS and DISK DISSIPATION. / Argiroffi, Costanza; Argiroffi, Costanza; Gorti, Uma; Pascucci, Ilaria; Principe, David A.; Kastner, Joel H.; Stelzer, Beate; Punzi, Kristina.

In: THE ASTRONOMICAL JOURNAL, Vol. 152, 2016, pag. 3-.

Risultato della ricerca: Article

Argiroffi, C, Argiroffi, C, Gorti, U, Pascucci, I, Principe, DA, Kastner, JH, Stelzer, B & Punzi, K 2016, 'M STARS in the TW HYA ASSOCIATION: STELLAR X-RAYS and DISK DISSIPATION', THE ASTRONOMICAL JOURNAL, vol. 152, pagg. 3-.
Argiroffi C, Argiroffi C, Gorti U, Pascucci I, Principe DA, Kastner JH e altri. M STARS in the TW HYA ASSOCIATION: STELLAR X-RAYS and DISK DISSIPATION. THE ASTRONOMICAL JOURNAL. 2016;152:3-.
Argiroffi, Costanza ; Argiroffi, Costanza ; Gorti, Uma ; Pascucci, Ilaria ; Principe, David A. ; Kastner, Joel H. ; Stelzer, Beate ; Punzi, Kristina. / M STARS in the TW HYA ASSOCIATION: STELLAR X-RAYS and DISK DISSIPATION. In: THE ASTRONOMICAL JOURNAL. 2016 ; Vol. 152. pagg. 3-.
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abstract = "To investigate the potential connection between the intense X-ray emission from young low-mass stars and the lifetimes of their circumstellar planet-forming disks, we have compiled the X-ray luminosities (L X) of M stars in the ∼8 Myr old TW Hya Association (TWA) for which X-ray data are presently available. Our investigation includes analysis of archival Chandra data for the TWA binary systems TWA 8, 9, and 13. Although our study suffers from poor statistics for stars later than M3, we find a trend of decreasing with decreasing T eff for TWA M stars, wherein the earliest-type (M0-M2) stars cluster near and then decreases, and its distribution broadens, for types M4 and later. The fraction of TWA stars that display evidence for residual primordial disk material also sharply increases in this same (mid-M) spectral type regime. This apparent anticorrelation between the relative X-ray luminosities of low-mass TWA stars and the longevities of their circumstellar disks suggests that primordial disks orbiting early-type M stars in the TWA have dispersed rapidly as a consequence of their persistent large X-ray fluxes. Conversely, the disks orbiting the very lowest-mass pre-MS stars and pre-MS brown dwarfs in the Association may have survived because their X-ray luminosities and, hence, disk photoevaporation rates are very low to begin with, and then further decline relatively early in their pre-MS evolution.",
keywords = "circumstellar matter; planets and satellites: formation; stars: formation; stars: pre-main sequence; Astronomy and Astrophysics; Space and Planetary Science",
author = "Costanza Argiroffi and Costanza Argiroffi and Uma Gorti and Ilaria Pascucci and Principe, {David A.} and Kastner, {Joel H.} and Beate Stelzer and Kristina Punzi",
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T1 - M STARS in the TW HYA ASSOCIATION: STELLAR X-RAYS and DISK DISSIPATION

AU - Argiroffi, Costanza

AU - Argiroffi, Costanza

AU - Gorti, Uma

AU - Pascucci, Ilaria

AU - Principe, David A.

AU - Kastner, Joel H.

AU - Stelzer, Beate

AU - Punzi, Kristina

PY - 2016

Y1 - 2016

N2 - To investigate the potential connection between the intense X-ray emission from young low-mass stars and the lifetimes of their circumstellar planet-forming disks, we have compiled the X-ray luminosities (L X) of M stars in the ∼8 Myr old TW Hya Association (TWA) for which X-ray data are presently available. Our investigation includes analysis of archival Chandra data for the TWA binary systems TWA 8, 9, and 13. Although our study suffers from poor statistics for stars later than M3, we find a trend of decreasing with decreasing T eff for TWA M stars, wherein the earliest-type (M0-M2) stars cluster near and then decreases, and its distribution broadens, for types M4 and later. The fraction of TWA stars that display evidence for residual primordial disk material also sharply increases in this same (mid-M) spectral type regime. This apparent anticorrelation between the relative X-ray luminosities of low-mass TWA stars and the longevities of their circumstellar disks suggests that primordial disks orbiting early-type M stars in the TWA have dispersed rapidly as a consequence of their persistent large X-ray fluxes. Conversely, the disks orbiting the very lowest-mass pre-MS stars and pre-MS brown dwarfs in the Association may have survived because their X-ray luminosities and, hence, disk photoevaporation rates are very low to begin with, and then further decline relatively early in their pre-MS evolution.

AB - To investigate the potential connection between the intense X-ray emission from young low-mass stars and the lifetimes of their circumstellar planet-forming disks, we have compiled the X-ray luminosities (L X) of M stars in the ∼8 Myr old TW Hya Association (TWA) for which X-ray data are presently available. Our investigation includes analysis of archival Chandra data for the TWA binary systems TWA 8, 9, and 13. Although our study suffers from poor statistics for stars later than M3, we find a trend of decreasing with decreasing T eff for TWA M stars, wherein the earliest-type (M0-M2) stars cluster near and then decreases, and its distribution broadens, for types M4 and later. The fraction of TWA stars that display evidence for residual primordial disk material also sharply increases in this same (mid-M) spectral type regime. This apparent anticorrelation between the relative X-ray luminosities of low-mass TWA stars and the longevities of their circumstellar disks suggests that primordial disks orbiting early-type M stars in the TWA have dispersed rapidly as a consequence of their persistent large X-ray fluxes. Conversely, the disks orbiting the very lowest-mass pre-MS stars and pre-MS brown dwarfs in the Association may have survived because their X-ray luminosities and, hence, disk photoevaporation rates are very low to begin with, and then further decline relatively early in their pre-MS evolution.

KW - circumstellar matter; planets and satellites: formation; stars: formation; stars: pre-main sequence; Astronomy and Astrophysics; Space and Planetary Science

UR - http://hdl.handle.net/10447/229163

UR - http://iopscience.iop.org/article/10.3847/0004-6256/152/1/3/pdf

M3 - Article

VL - 152

SP - 3-

JO - Astronomical Journal

JF - Astronomical Journal

SN - 0004-6256

ER -