2011A&A...535A..99M


C.D.S. - SIMBAD4 rel 1.7 - 2021.03.01CET21:41:47

2011A&A...535A..99M - Astronomy and Astrophysics, volume 535A, 99-99 (2011/11-1)

Accretion rates and accretion tracers of Herbig Ae/Be stars.

MENDIGUTIA I., CALVET N., MONTESINOS B., MORA A., MUZEROLLE J., EIROA C., OUDMAIJER R.D. and MERIN B.

Abstract (from CDS):

The scarcity of accretion rate estimates and accretion tracers available for Herbig Ae/Be (HAeBe) stars contrasts with the extensive studies for lower mass objects. This work aims to derive accretion rates from the UV Balmer excess for a sample of 38 HAeBe stars. We look for possible empirical correlations with the strength of the Hα, [OI]6300, and Brγ emission lines. Shock modelling within the context of magnetospheric accretion (MA) was applied to each star. We obtained the accretion rates from the excess in the Balmer discontinuity, derived from mean values of multi-epoch Johnson's UB photometry. The accretion rates were related to both mean Hα luminosities, Hα 10% widths, and [OI]6300 luminosities from simultaneous spectra, and to Brγ luminosities from the literature. The typical -median- mass accretion rate is 2x10–7M/yr in our sample, 36% of the stars showing values ≤10–7M/yr, 35% between 10–7 and 10–6, and 29%>10–6M/yr. The model fails to reproduce the large Balmer excesses shown by the four hottest stars (T*>12000K). When accretion is related to the stellar masses and luminosities (1≤M*/M≤6; 2≤L*/L≤103), we derive {dot}(M)acc∝M*5 and Lacc∝L*1.2, with scatter. Empirical calibrations relating the accretion and the Hα, [OI]6300, and Brγ luminosities are provided. The slopes in our expressions are slightly shallower than those for lower mass stars, but the difference is within the uncertainties, except for the [OI]6300 line. The Hα 10% width is uncorrelated with {dot}(M)acc, unlike for the lower mass regime. The mean Hα width shows higher values as the projected rotational velocities of HAe stars increase, which agrees with MA. The accretion rate variations in the sample are typically lower than 0.5dex on timescales of days to months. Our data suggest that the changes in the Balmer excess are uncorrelated to the simultaneous changes of the line luminosities. The Balmer excesses and Hα line widths of HAe stars can be interpreted within the context of MA, which is not the case for several HBes. The steep trend relating {dot}(M)acc and M* can be explained from the mass-age distribution characterizing HAeBe stars. The line luminosities used for low-mass objects are also valid to estimate typical accretion rates for the intermediate-mass regime under similar empirical expressions. However, we suggest that several of these calibrations are driven by the stellar luminosity.

Abstract Copyright:

Journal keyword(s): circumstellar matter - accretion, accretion disks - stars: pre-main sequence - protoplanetary disks - stars: activity - line: formation

Simbad objects: 38

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Number of rows : 38

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 V* VX Cas Ae* 00 31 30.6816836826 +61 58 50.982831889 11.83 11.59 10.50 11.19 10.94 A0Vep 128 0
2 V* XY Per Ae* 03 49 36.3362509899 +38 58 55.551266650 12.12 10.14 9.58 9.54 8.40 A2II+B6 142 0
3 V* RY Tau Or* 04 21 57.4132838427 +28 26 35.533990877 10.82 10.34 9.30 9.67 8.87 K1IV/Ve 661 1
4 HD 31648 Ae* 04 58 46.2654165113 +29 50 36.990341242 7.84 7.78 7.62 7.76 7.43 A5Vep 411 0
5 V* UX Ori Ae* 05 04 29.9881676817 -03 47 14.288047238 10.25 10.93 8.70 9.62 9.43 A4IVe 338 1
6 V* V1366 Ori Ae* 05 16 00.4764811920 -09 48 35.394685295 10.19 10.16 9.84 9.77 9.63 B9.5V 168 0
7 HD 34700 TT* 05 19 41.4088548858 +05 38 42.777125431 9.75 9.788 9.15 8.80 8.47 G0IVe 74 0
8 HD 287841 Y*O 05 24 42.8031051407 +01 43 48.249517233 10.55 10.45 10.17 9.99 9.80 A8V 92 0
9 V* CO Ori Or* 05 27 38.3352 +11 25 38.923 12.96 12.33 10.30 10.33 9.63 F7Ve 158 0
10 V* HK Ori Ae* 05 31 28.0451235474 +12 09 10.149849783 11.82 12.06 11.10 11.02 10.56 A2?e+G0?e 178 1
11 V* RY Ori Or* 05 32 09.9419985443 -02 49 46.769539985 12.62 12.76 10.80 10.82 10.34 F7 52 0
12 V* NV Ori Ae* 05 35 31.3684708885 -05 33 08.871090196 10.36 10.21 8.70 9.48 9.22 F6IIIe 92 0
13 V* T Ori Ae* 05 35 50.4483740019 -05 28 34.923375739 12.724 11.637 11.248 10.09 10.043 A3IVeb 232 0
14 V* CQ Tau Ae* 05 35 58.4671238887 +24 44 54.086375712 11.290 10.780 10.000   8.33 F5IVe 265 0
15 V* BF Ori Ae* 05 37 13.2623698298 -06 35 00.565420577 10.37 10.00 9.69 10.06 9.31 A7III 272 0
16 V* RR Tau Ae* 05 39 30.5114685049 +26 22 26.961204895 11.64 12.09 11.28 10.58 10.17 A0:IVe 217 0
17 V* V350 Ori Y*O 05 40 11.7641189614 -09 42 11.085315699 12.74 12.08 11.42 11.38 10.96 A7V 68 0
18 V* VY Mon Ae* 06 31 06.9180562526 +10 26 04.982093681 16.65 15.45 13.70 12.49 11.00 A5:Vep 89 0
19 V* R Mon Ae* 06 39 09.9538710861 +08 44 09.559404231 10.76 12.46 11.85 10.96 10.25 B8IIIe 506 0
20 HD 58647 Em* 07 25 56.0988044433 -14 10 43.548997982 6.81 6.92 6.85 6.73 6.73 B9IV 77 0
21 HD 141569 Y*O 15 49 57.7484743862 -03 55 16.344023102 7.22 7.20 7.12 7.00 7.04 A2VekB9mB9(_lB) 480 0
22 HD 142666 TT* 15 56 40.0222941557 -22 01 40.004849949 9.41 9.37 8.82 8.31 8.01 F0V_sh 225 0
23 HD 144432 Ae* 16 06 57.9530266912 -27 43 09.758016578 8.47 8.53 8.19 7.82 7.53 A9/F0V 218 1
24 HD 150193 Be* 16 40 17.9242900066 -23 53 45.192676418 9.69 9.32 8.79 8.41   B9.5Ve 296 0
25 EM* AS 220 Ae* 17 10 08.1238 -27 15 18.801 12.86 12.79 12.22 12.03 10.82 A6Ve+G5Ve 132 0
26 * c Oph Be* 17 31 24.9541340 -23 57 45.513592 4.75 4.81 4.81 4.74 4.72 A0V 257 0
27 HD 163296 Ae* 17 56 21.2882188601 -21 57 21.872343282 7.00 6.93 6.85 6.86 6.67 A1Vep 840 0
28 V* VV Ser Ae* 18 28 47.8619658319 +00 08 39.924642619 12.99 12.63 11.80 11.01 10.24 A5Ve 232 0
29 HD 179218 Ae* 19 11 11.2540715594 +15 47 15.632212730 7.55 7.476 7.39 7.25 7.21 A0Ve 225 0
30 V* WW Vul Ae* 19 25 58.7494596284 +21 12 31.333220807 11.46 10.99 10.25 10.38 10.12 A2IVe 216 0
31 V* PX Vul Or* 19 26 40.2533631097 +23 53 50.777553057 12.56 12.57 11.83 10.90 10.30 F3Ve 50 0
32 HD 190073 Ae* 20 03 02.5098091524 +05 44 16.658081203 7.91 7.86 7.73   7.65 A2IVe 232 0
33 EM* LkHA 224 Ae* 20 20 29.3500765489 +41 21 28.448014439 14.82 14.08 12.93 12.05 11.08 A4:Ve 92 0
34 EM* AS 442 Ae* 20 47 37.4658048789 +43 47 24.973275249 11.90 11.56 10.90 10.18 9.95 B8Ve 84 0
35 EM* LkHA 234 Ae* 21 43 06.8214472757 +66 06 54.199354231 13.65 13.61 12.73 11.98 11.20 B5Ve 278 0
36 V* BH Cep Ae* 22 01 42.8726806026 +69 44 36.423728031 12.18 11.54 11.01 10.62 10.32 F5IIIe 57 0
37 V* BO Cep Ae* 22 16 54.0590233441 +70 03 44.984949208 11.86 11.98 11.55 11.16 10.84 F5Ve 62 0
38 V* SV Cep Ae* 22 21 33.2175224577 +73 40 27.096415978 11.40 11.25 10.35 10.28 10.08 A2IVe 124 0

    Equat.    Gal    SGal    Ecl

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2021.03.01-21:41:47

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