2015A&A...574A..44B


C.D.S. - SIMBAD4 rel 1.7 - 2019.10.14CEST14:04:00

2015A&A...574A..44B - Astronomy and Astrophysics, volume 574A, 44-44 (2015/2-1)

Mass accretion rates from multiband photometry in the Carina Nebula: the case of Trumpler 14.

BECCARI G., DE MARCHI G., PANAGIA N., VALENTI E., CARRARO G., ROMANIELLO M., ZOCCALI M. and WEIDNER C.

Abstract (from CDS):

We present a study of the mass accretion rates of pre-main sequence (PMS) stars in the cluster Trumpler 14 (Tr 14) in the Carina Nebula. Using optical multiband photometry we were able to identify 356 PMS stars showing Hα excess emission with equivalent width EW(Hα)>20Å. We interpret this observational feature as an indication that these objects are still actively accreting gas from their circumstellar medium. From a comparison of the HR diagram with PMS evolutionary models we derive ages and masses of the PMS stars. We find that most of the PMS objects are younger than 10Myr with a median age of ∼3Myr. Surprisingly, we also find that ∼20% of the mass accreting objects are older than 10Myr. For each PMS star in Trumpler 14 we determine the mass accretion rate ({dot}(M)acc) and discuss its dependence on mass and age. We finally combine the optical photometry with near-IR observations to build the spectral energy distribution (SED) for each PMS star in Tr 14. The analysis of the SEDs suggests the presence of transitional discs in which a large amount of gas is still present and sustains accretion onto the PMS object at ages older than 10Myr. Our results, discussed in light of recent recent discoveries with Herschel of transitional discs containing a massive gas component around the relatively old PMS stars TWHydrae, 49Ceti, and HD95086, support a new scenario n which old and evolved debris discs still host a significant amount of gas.

Abstract Copyright:

Journal keyword(s): accretion, accretion disks - stars: pre-main sequence

Simbad objects: 20

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Number of rows : 20

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2019
#notes
1 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 9082 1
2 NGC 346 Cl* 00 59 05.090 -72 10 33.24           ~ 441 0
3 NGC 602 Cl* 01 29 32.133 -73 33 38.13     13.018     ~ 77 1
4 * 49 Cet PM* 01 34 37.7788265080 -15 40 34.898112472   5.667 5.607   5.54 A1V 229 0
5 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 5369 1
6 NAME Tau-Aur Region SFR 04 30 +25.0           ~ 1177 1
7 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14316 1
8 RMC 136 Cl* 05 38 42.396 -69 06 03.36   9.63 9.50     ~ 1674 2
9 Cl Trumpler 14 OpC 10 43 56 -59 33.0   5.70 5.5     ~ 411 0
10 NGC 3372 HII 10 44 19.0 -59 53 21           ~ 866 2
11 C 1042-593 OpC 10 44 39.00 -59 33 36.0     6.8     ~ 56 0
12 * eta Car Em* 10 45 03.5455050 -59 41 03.951060 6.37 7.034 6.21 4.90 4.41 OBepec 2148 0
13 Cl Trumpler 16 OpC 10 45 10 -59 43.0   5.35 5.0     ~ 414 0
14 HD 95086 * 10 57 03.0216129217 -68 40 02.446874288   7.60 7.36     A8III 114 1
15 V* TW Hya TT* 11 01 51.9054298616 -34 42 17.031550898   11.94 10.50 10.626 9.18 K6Ve 1440 1
16 NGC 3603 HII 11 15 24 -61 15.0           ~ 919 2
17 M 16 OpC 18 18 48 -13 48.4   6.58 6.0     ~ 918 2
18 NGC 6823 OpC 19 43 09 +23 18.0   7.71 7.1     ~ 247 2
19 IC 1396 OpC 21 39 00 +57 29.4           ~ 438 1
20 Ass Cep OB 2 As* 21 51 +60.0           ~ 276 0

    Equat.    Gal    SGal    Ecl

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2019.10.14-14:04:00

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