2012A&A...543A..59M


Query : 2012A&A...543A..59M

2012A&A...543A..59M - Astronomy and Astrophysics, volume 543A, 59-59 (2012/7-1)

Accretion-related properties of Herbig Ae/Be stars. Comparison with T Tauris.

MENDIGUTIA I., MORA A., MONTESINOS B., EIROA C., MEEUS G., MERIN B. and OUDMAIJER R.D.

Abstract (from CDS):

The mass accretion rate ({dot}(M)acc) is a key parameter that has not accurately been determined for a wide sample of Herbig Ae/Be (HAeBe) stars until recently. We look for trends relating {dot}(M)acc and the stellar ages (t), spectral energy distributions (SEDs), and disk masses for a sample of 38 HAeBe stars, comparing them to analogous correlations found for classical T Tauri stars. Our goal is ultimately to shed light on the timescale and physical processes that drive the evolution of intermediate-mass pre-main sequence objects. Mass accretion rates obtained by us in a previous work were related to several stellar and disk parameters: the age of the stars was compiled from the literature, SEDs were classified according to their shape and the wavelength where the IR excess starts, near- and mid-IR colour excesses were computed, and disk masses were estimated from mm fluxes. {dot}(M)acc decreases with the stellar age, showing a dissipation timescale τ=1.3+1.0–0.5Myr from an exponential law fit, while a power law yields {dot}(M)acc(t)∝t–η, with η=1.8+1.4–0.7. This result is based on our whole HAeBe sample (1-6M), but the accretion rate decline most probably depends on smaller stellar mass bins. The near-IR excess is higher and starts at shorter wavelengths (J and H bands) for the strongest accretors. Active and passive disks are roughly divided by ∼2x10–7M/yr. The mid-IR excess and the SED shape from the Meeus et al. (2001A&A...365..476M) classification are not correlated with {dot}(M)acc. Concerning disk masses, we find {dot}(M)acc∝Mdisk^1.1 ±0.3^. Most stars in our sample with signs of inner dust dissipation typically show accretion rates ten times lower and disk masses three times smaller than the remaining objects. The trends relating {dot}(M)acc with the near-IR excess and Mdisk extend those found for T Tauri stars, and are consistent with viscous disk models. The differences in the inner gas dissipation timescale, and the relative position of the stars with signs of inner dust clearing in the {dot}(M)acc-Mdisk plane, could be suggesting a slightly faster evolution, and that a different process - such as photoevaporation - plays a more relevant role in dissipating disks in the HAeBe regime compared to T Tauri stars. Our conclusions must consider the mismatch between the disk mass estimates from mm fluxes and the disk mass estimates from accretion, which we also find in HAeBe stars.

Abstract Copyright:

Journal keyword(s): stars: pre-main sequence - stars: variables: T Tauri, Herbig Ae/Be - accretion, accretion disks - circumstellar matter - protoplanetary disks

Simbad objects: 41

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Number of rows : 41
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 V* VX Cas Ae* 00 31 30.6818495040 +61 58 50.984946300 11.83 11.59 10.50 11.19 10.94 A0Vep 131 0
2 IC 1795 HII 02 25 43.5 +62 06 13           ~ 236 0
3 V* XY Per Ae* 03 49 36.3365862552 +38 58 55.548299928 12.12 10.14 9.58 9.54 8.40 A2II+B6 147 0
4 V* RY Tau Or* 04 21 57.4092550080 +28 26 35.555316612 10.82 10.34 9.30 9.67 8.87 K1IV/Ve 684 1
5 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 4096 0
6 HD 31648 Ae* 04 58 46.2655706952 +29 50 36.987625680 7.84 7.78 7.62 7.76 7.43 A5Vep 474 0
7 V* UX Ori Ae* 05 04 29.9878898040 -03 47 14.286732072 10.25 10.93 8.70 9.62 9.43 A4IVe 353 1
8 V* V1366 Ori Ae* 05 16 00.4765181328 -09 48 35.393784012 10.19 10.16 9.84 9.77 9.63 B9.5V 192 0
9 HD 34700 SB* 05 19 41.4089390784 +05 38 42.778590864 9.75 9.778 9.659 9.205 8.47 G0IVe 92 0
10 HD 287841 Y*O 05 24 42.8032369656 +01 43 48.249234516 10.55 10.45 10.17 9.99 9.80 A8V 101 0
11 V* CO Ori Or* 05 27 38.3386648 +11 25 38.974625 12.96 12.33 10.30 10.33 9.63 F7Ve 162 0
12 V* HK Ori Ae* 05 31 28.049808 +12 09 10.30212 11.82 12.235 11.716 11.632 10.56 A2?e+G0?e 187 1
13 V* RY Ori Or* 05 32 09.9419233368 -02 49 46.770599784 12.62 12.76 10.80 10.82 10.34 F7 57 0
14 V* NV Ori Ae* 05 35 31.3686116448 -05 33 08.872027056 10.36 10.21 8.70 9.48 9.22 F6IIIe 98 0
15 V* T Ori Ae* 05 35 50.4482802768 -05 28 34.925254536 12.724 11.637 11.248 10.09 10.043 A3IVeb 243 0
16 V* CQ Tau Ae* 05 35 58.4666264136 +24 44 54.091450572 11.290 10.780 10.000   8.33 F5IVe 286 0
17 V* BF Ori Ae* 05 37 13.2623828280 -06 35 00.568242528 10.37 10.00 9.69 10.06 9.31 A7III 282 0
18 V* RR Tau Ae* 05 39 30.5115918672 +26 22 26.967444996 11.64 12.09 11.28 10.58 10.17 A0:IVe 222 0
19 V* V350 Ori LP* 05 40 11.7638894112 -09 42 11.086012692 12.74 12.08 11.42 11.38 10.96 A7V 74 0
20 V* VY Mon Ae* 06 31 06.9271406952 +10 26 04.952351076 16.65 15.45 13.70 12.49 11.00 A5:Vep 93 0
21 V* R Mon Ae* 06 39 09.9542000448 +08 44 09.539482632 10.76 12.46 11.85 10.96 10.25 B8IIIe 511 0
22 HD 58647 Em* 07 25 56.0985504216 -14 10 43.548632256 6.81 6.92 6.85 6.73 6.73 B9IV 85 0
23 HD 141569 Y*O 15 49 57.7482550392 -03 55 16.341617064 7.22 7.20 7.12 7.00 7.04 A2VekB9mB9(_lB) 511 0
24 HD 142666 TT* 15 56 40.0221861696 -22 01 40.005872148 9.41 9.37 8.82 8.31 8.01 F0V_sh 246 0
25 HD 144432 Ae* 16 06 57.9533126832 -27 43 09.760564056 8.47 8.53 8.19 7.82 7.53 A9/F0V 230 1
26 HD 150193 Be* 16 40 17.9243127240 -23 53 45.193372692 9.69 9.32 8.79 8.41   B9.5Ve 307 0
27 EM* AS 220 Ae* 17 10 08.1238 -27 15 18.801 12.86 12.79 12.22 12.03 10.82 A6Ve+G5Ve 138 0
28 * c Oph Be* 17 31 24.9538710166 -23 57 45.514802684 4.75 4.81 4.81 4.74 4.72 A0V 266 0
29 HD 163296 Ae* 17 56 21.2881851168 -21 57 21.871819008 7.00 6.93 6.85 6.86 6.67 A1Vep 1003 0
30 V* VV Ser Ae* 18 28 47.8620017808 +00 08 39.923474964 12.99 12.63 11.80 11.01 10.24 A5Ve 242 0
31 NAME Serpens Cloud SFR 18 29 49 +01 14.8           ~ 1049 2
32 HD 179218 Ae* 19 11 11.2538919456 +15 47 15.636008472 7.55 7.476 7.39 7.25 7.21 A0Ve 241 0
33 V* WW Vul Ae* 19 25 58.7494120560 +21 12 31.333658616 11.46 10.99 10.25 10.38 10.12 A2IVe 221 0
34 V* PX Vul Or* 19 26 40.2532914312 +23 53 50.782579116 12.56 12.57 11.83 10.90 10.30 F3Ve 53 0
35 HD 190073 Ae* 20 03 02.5098474264 +05 44 16.660712904 7.91 7.86 7.73   7.65 A2IVe 244 0
36 EM* LkHA 224 Ae* 20 20 29.3503944888 +41 21 28.410038964 14.82 14.08 12.93 12.05 11.08 A4:Ve 99 0
37 EM* AS 442 Ae* 20 47 37.4657848584 +43 47 24.975739896 11.90 11.56 10.90 10.18 9.95 B8Ve 90 0
38 EM* LkHA 234 Ae* 21 43 06.8218113480 +66 06 54.202272804 13.65 13.61 12.73 11.98 11.20 B5Ve 283 0
39 V* BH Cep Ae* 22 01 42.8723960712 +69 44 36.426918696 12.18 11.54 11.01 10.62 10.32 F5IIIe 61 0
40 V* BO Cep Ae* 22 16 54.0583196880 +70 03 44.988517332 11.86 11.98 11.55 11.16 10.84 F5Ve 67 0
41 V* SV Cep Ae* 22 21 33.2166238512 +73 40 27.097678812 11.40 11.25 10.35 10.28 10.08 A2IVe 128 0

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2023.02.01-20:00:36

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