2011A&A...526A.104C


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.10CEST02:55:11

2011A&A...526A.104C - Astronomy and Astrophysics, volume 526A, 104-104 (2011/2-1)

Multiwavelength diagnostics of accretion in an X-ray selected sample of CTTSs.

CURRAN R.L., ARGIROFFI C., SACCO G.G., ORLANDO S., PERES G., REALE F. and MAGGIO A.

Abstract (from CDS):

High resolution X-ray spectroscopy has revealed soft X-rays from high density plasma in classical T Tauri stars (CTTSs), probably arising from the accretion shock region. However, the mass accretion rates derived from the X-ray observations are consistently lower than those derived from UV/optical/NIR studies. We aim to test the hypothesis that the high density soft X-ray emission originates from accretion by analysing, in a homogeneous manner, optical accretion indicators for an X-ray selected sample of CTTSs. We analyse optical spectra of the X-ray selected sample of CTTSs and calculate the accretion rates based on measuring the Hα, Hβ, Hγ, HeII 4686Å, HeI 5016Å, HeI 5876Å, OI 6300Å, and HeI 6678Å equivalent widths. In addition, we also calculate the accretion rates based on the full width at 10% maximum of the Hα line. The different optical tracers of accretion are compared and discussed. The derived accretion rates are then compared to the accretion rates derived from the X-ray spectroscopy. We find that, for each CTTS in our sample, the different optical tracers predict mass-accretion rates that agree within the errors, albeit with a spread of ≃1 order of magnitude. Typically, mass-accretion rates derived from Hα and HeI 5876 Å are larger than those derived from Hβ, Hγ, and OI. In addition, the Hα full width at 10%, whilst a good indicator of accretion, may not accurately measure the mass-accretion rate. When the optical mass-accretion rates are compared to the X-ray derived mass-accretion rates, we find that: a) the latter are always lower (but by varying amounts); b) the latter range within a factor of ≃2 around 2x10–10M/yr, despite the former spanning a range of ≃3 orders of magnitude. We suggest that the systematic underestimate of the X-ray derived mass-accretion rates could depend on the density distribution inside the accretion streams, where the densest part of the stream is not visible in the X-ray band because of the absorption by the stellar atmosphere. We also suggest that a non-negligible optical depth of X-ray emission lines produced by post-shock accreting plasma may explain the almost constant mass-accretion rates derived in X-rays if the effect is larger in stars with higher optical mass-accretion rates.

Abstract Copyright:

Journal keyword(s): accretion, accretion disks - circumstellar matter - stars: pre-main sequence - techniques: spectroscopic

Simbad objects: 16

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Number of rows : 16

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 V* BP Tau Or* 04 19 15.8342975037 +29 06 26.929456808   13.13 12.12 11.89   K5/7Ve 599 0
2 NAME T Tau Sa *i* 04 21 59.371 +19 32 05.95           ~ 65 0
3 NAME T Tau Sb *i* 04 21 59.371 +19 32 05.95           M1 70 0
4 V* T Tau Or* 04 21 59.4323326335 +19 32 06.439974179   11.01 9.30 9.80   K0IV/Ve 1249 2
5 NAME T Tau N *i* 04 21 59.433 +19 32 06.42   11.22 10.12 9.80   K1.5 164 1
6 NAME Tau-Aur Complex SFR 04 30 +25.0           ~ 1217 0
7 V* TW Hya TT* 11 01 51.9054298616 -34 42 17.031550898   11.94 10.50 10.626 9.18 K6Ve 1532 1
8 NAME TW Hya Association As* 11 01.9 -34 42           ~ 819 0
9 TWA 3 ** 11 10 27.894072 -37 31 51.96612   13.53 12.05 11.61 9.29 M4Ve+M4Ve 200 0
10 TWA 3A TT* 11 10 27.9117558304 -37 31 51.529219753   14.04 12.57   9.10 M4Ve 185 0
11 NAME Lower Centaurus Crux As* 12 19 -57.1           ~ 354 1
12 CPD-68 1894 TT* 13 22 07.5420267499 -69 38 12.216304202   11.38 10.393   9.117 K1Ve 128 0
13 V* RU Lup Or* 15 56 42.3109948086 -37 49 15.473469159 9.27 10.07 9.60     K7/M0e 382 0
14 EM* SR 9 Or* 16 27 40.2858402419 -24 22 04.132012501   12.91 11.533 11.11 10.00 K5e 249 0
15 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3027 0
16 HD 319139 BY* 18 14 10.4818974563 -32 47 34.516106830   11.47 10.68   9.11 K5+K7 290 0

    Equat.    Gal    SGal    Ecl

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2020.07.10-02:55:11

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