2002A&A...387..977F


Query : 2002A&A...387..977F

2002A&A...387..977F - Astronomy and Astrophysics, volume 387, 977-992 (2002/6-1)

The history of mass dispersal around Herbig Ae/Be stars.

FUENTE A., MARTIN-PINTADO J., BACHILLER R., RODRIGUEZ-FRANCO A. and PALLA F.

Abstract (from CDS):

We present a systematic study of the material surrounding intermediate-mass stars. Our sample includes 34 Herbig Ae/Be (HAEBE) stars of different ages and luminosities. This is a quite complete representation of the whole class of HAEBE stars and consequently, our conclusions should have a solid statistical meaning. In addition, we have observed 2 intermediate-mass protostars and included published data on 15 protostellar objects in order to determine the evolution of the circumstellar material in the early stages of stellar evolution. All the HAEBE stars have been classified according with the three Types already defined in Fuente et al. (1998A&A...334..253F): Type I stars are immersed in a dense clump and have associated bipolar outflows, their ages are ∼0.1Myr; Type II stars are still immersed in the molecular cloud though not in a dense clump, their ages are between ∼a few 0.1 to ∼a few Myr; Type III stars have completely dispersed the surrounding material and are located in a cavity of the molecular cloud, their ages are >1Myr. Our observations are used to reconstruct the evolution of the circumstellar material around intermediate-mass stars and investigate the mass dispersal mechanisms at the different stages of the stellar evolution. Our results can be summarized as follows: intermediate-mass stars disperse ≥90% of the mass of the parent clump during the protostellar phase. During this phase, the energetic outflows sweep out the gas and dust forming a biconical cavity while the equatorial material is infalling to feed the circumstellar disk and eventually the protostar. In this way, the density structure of the parent clump remains well described by a density law n∝rβ with -2<β←1 although a large fraction of the mass is dispersed. In ∼a few 0.1Myr, the star becomes visible and the outflow fades. Some material is dispersed from ∼a few 0.1 to ≥1Myr. Since the outflow declines and the stars are still too cold to generate UV photons, stellar winds are expected to be the only dispersal mechanism at work. In 1Myr an early-type star (B0-B5) and in ≥1 to 10Myr a late-type star (later than B6) meets the ZAMS. Now the star is hot enough to produce UV photons and starts excavating the molecular cloud. Significant differences exist between early-type and late-type stars at this evolutionary stage. Only early-type stars are able to create large (R>0.08 pc) cavities in the molecular cloud, producing a dramatic change in the morphology of the region. This difference is easily understood if photodissociation plays an important role in the mass dispersal around these objects.

Abstract Copyright:

Journal keyword(s): stars: formation - stars: pre-main sequence - ISM: abundances - ISM: molecules

Simbad objects: 57

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Number of rows : 57
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 EM* LkHA 198 Ae* 00 11 25.8510585961 +58 49 28.677348580   14.65 13.79 14.03   B9e 222 0
2 LBN 119.83-06.05 MoC 00 28 43.5075 +56 41 56.868           ~ 65 0
3 BD+61 154 Ae* 00 43 18.2564711093 +61 54 40.138272968 10.83 11.13 10.60     B8eq 195 1
4 NAME RNO 6NW MCld MoC 02 15 57.1 +55 28 12           A5 4 0
5 HBC 334 Em* 02 16 30.7114261492 +55 23 00.140497532   14.92 14.32 14.52   B3 31 0
6 NAME LDN 1455 IRS 1 cor 03 27 39.08 +30 13 03.1           ~ 146 0
7 NAME HH 7-11 FIR 03 29 03.9 +31 16 06           ~ 337 0
8 IRAS 03445+3242 Y*O 03 47 41.603 +32 51 43.79           ~ 180 0
9 V* V892 Tau Ae* 04 18 40.6120892867 +28 19 15.641672501   16.6 14.69 14.35   A0Ve 271 0
10 RAFGL 5123 Y*O 04 31 34.07736 +18 08 04.9020           K3V/M3III 822 0
11 V* AB Aur Ae* 04 55 45.8459978418 +30 33 04.293281305 7.20 7.16 7.05 6.96 6.70 A0Ve 960 2
12 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 180 1
13 HD 245185 Ae* 05 35 09.6040600795 +10 01 51.465846371 10.05 10.07 9.93     A0Vae 109 0
14 V* T Ori Ae* 05 35 50.4483740019 -05 28 34.923375739 12.724 11.637 11.248 10.09 10.043 A3IVeb 234 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 * ome Ori Be* 05 39 11.1463172 +04 07 17.279475 3.73 4.48 4.59 4.57 4.67 B3Ve 392 1
17 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
18 NGC 2071 RNe 05 47 10 +00 18.0           ~ 617 1
19 NAME G 192.16 cor 05 58 13.53 +16 31 58.3           ~ 21 1
20 HD 250550 Ae* 06 01 59.9894900068 +16 30 56.724889160   9.60 9.593 9.64   B9e 235 1
21 NAME Mon R2 HII 06 07 47.58 -06 22 42.6           ~ 674 2
22 EM* LkHA 208 Ae* 06 07 49.5332262163 +18 39 26.493880740   11.78 11.30 11.39   F0Ve 119 1
23 EM* MWC 137 Ae* 06 18 45.5220562759 +15 16 52.242746933 12.89 13.30 13.759 11.67 10.31 sgB[e]d 228 1
24 EM* LkHA 215 Ae* 06 32 41.7734957477 +10 09 34.205635971 11.41 11.28 10.70     B7IIne 122 0
25 HD 259431 Ae* 06 33 05.1905483916 +10 19 19.987469692 8.39 8.95 8.72     B6ep 268 1
26 EM* LkHA 25 Ae* 06 40 44.6381481431 +09 48 02.146205543 12.745 13.03 12.88 12.545 12.386 B4Ve 131 0
27 HD 52721 Ae* 07 01 49.50977 -11 18 03.3219 5.88 6.65 6.59 7.52   B2Vne 204 0
28 EM* LkHA 218 Ae* 07 02 42.5311084174 -11 26 11.826251745   13 11.63     A0e 61 0
29 V* Z CMa Ae* 07 03 43.1588002461 -11 33 06.230351311 10.51 9.99 8.80     B5/8eq+F5/7 537 3
30 HD 53367 Ae* 07 04 25.5189757244 -10 27 15.613478141 6.81 7.40 6.96 7.92   B0IV/Ve 307 0
31 BD+36 2322B PM* 12 57 39.3125173002 +35 13 19.148808620   14.80 13.16 12.939   M4.5V 90 1
32 BD+36 2322 BY* 12 57 40.2114201833 +35 13 30.069647793   12.2   10.137   M0V+M4/5V 218 1
33 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3195 1
34 IRAS 16293-2422 cor 16 32 22.56 -24 28 31.8           ~ 1104 1
35 NAME GGD 27 IRS RNe 18 19 12.0871543084 -20 47 50.895583646           ~ 26 1
36 EM* MWC 297 Ae* 18 27 39.5266257570 -03 49 52.136526892 15.57 14.34 12.31 11.34   B1.5Ve 271 0
37 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
38 NAME Serpens Cloud SFR 18 29 49 +01 14.8           ~ 976 2
39 Parsamian 21 Or* 19 29 00.849408 +09 38 43.39932   15.18 14.07 13.93   F5Iabe 82 0
40 IRAS 20126+4104 Y*O 20 14 25.8816186803 +41 13 36.869078243           B2.5-B0.5 406 0
41 RAFGL 2591 Y*O 20 29 25.03656 +40 11 20.3316           ~ 578 0
42 V* PV Cep Or* 20 45 53.9537161790 +67 57 38.678052612   19.27 17.46 15.98 14.60 A5 255 3
43 HD 200775 Ae* 21 01 36.9184805541 +68 09 47.770037306 7.34 7.754 7.427 8.13   B2Ve 520 0
44 BD+65 1637 Ae* 21 42 50.1799735837 +66 06 35.184005596 10.21 10.56 10.53 10.29   B3IV-Vne 148 1
45 NGC 7129 OpC 21 42 56 +66 06.2     11.5     ~ 238 0
46 EM* LkHA 234 Ae* 21 43 06.8214472757 +66 06 54.199354231 13.65 13.61 12.73 11.98 11.20 B5Ve 279 0
47 NAME NGC 7129 FIR 2 IR 21 44 01.5 +66 03 40           ~ 88 0
48 BD+46 3471 Ae* 21 52 34.0992388111 +47 13 43.600551484 10.72 10.56 10.15     A0.5IIIer 198 1
49 EM* LkHA 257 Ae* 21 54 18.7802039069 +47 12 09.667376789 15.195 13.87 13.16     B5/A2e 51 0
50 SH 2-140 OpC 22 19 07.8 +63 17 07           ~ 642 2
51 IRAS 22176+6303 Y*O 22 19 17.978 +63 18 52.92           ~ 590 0
52 EM* LkHA 233 Ae* 22 34 40.9923134958 +40 40 04.251892858   14.5       A7Ve 142 0
53 HD 216629 Ae* 22 53 15.6043627656 +62 08 45.000152794 9.83 9.93 9.36 9.31   B3IVe+A3 128 0
54 NAME Cepheus A SFR 22 56 17.9 +62 01 49           ~ 711 2
55 EM* AS 505 Ae* 23 05 07.4613720352 +62 15 36.502340613 10.09 11.5 10.9     B5Vep 59 0
56 EM* MWC 1080 Ae* 23 17 25.5890248379 +60 50 43.452566559   13.24 11.542     B0eq 310 0
57 Mol 160 Rad 23 40 54.5 +61 10 28           ~ 92 0

    Equat.    Gal    SGal    Ecl

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2021.07.25-19:05:10

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