1997A&AS..126..437H


C.D.S. - SIMBAD4 rel 1.7 - 2021.05.07CEST16:29:22

1997A&AS..126..437H - Astron. Astrophys., Suppl. Ser., 126, 437-469 (1997/December-2)

Spatial and kinematic properties of the forbidden emission line region of T Tauri stars.

HIRTH G.A., MUNDT R. and SOLF J.

Abstract (from CDS):

We have carried out a long-slit spectroscopic survey for 38 T Tauri stars (TTSs) to study the spatial and kinematic properties of their forbidden emission line (FEL) regions. With these observations we hope to provide more insight into the complex physical structure of the outflows from young stars on the smallest spatial scales observable by long-slit spectroscopy. Due to the differential nature of the observational method, information on the spatial properties (offset from the stellar continuum and spatial width) on sub-arcsec (sub-seeing) scales can be obtained. For most TTSs the [OI] λλ6300, 6363, [NII] λ6583 and [SII] λλ6716, 6731 lines have been investigated at a typical spatial resolution of 1.5'' and a velocity resolution of 20-50km/s. A sub-sample of 9 closeby stars (Haro 6-10, XZ Tau, UZ Tau E, HN Tau, DO Tau, DP Tau, UY Aur, RW Aur and V536 Aql) has been extensively studied and the direction of their outflows has been approximately determined by taking spectra at several slit position angles, if not known from emission-line CCD imaging. The spatial and kinematic properties of the FEL regions of these 9 TTSs are described in detail. Together with 3 additional stars discussed in the literature, a sample of 12 stars provides the basis for the following main results of our survey: The so-called high-velocity component (HVC) of the FELs (or gas of high velocity which presumably represents in many cases a HVC being blended with emission of lower velocity) is generally spatially more extended than the so-called low-velocity component (LVC, or gas near the stellar velocity). In the [SII] λ6731 line the centroid of the high-velocity gas is located typically at distances of 0.6'' from the TTS while for the low-velocity gas this value is smaller on average by more than a factor of 3. Comparing the spatial properties of the high-velocity gas among the investigated FELs, it turns out that the largest spatial width and the largest offset of the centroid from the star is usually observed in the [NII] λ6583 line, while the emission region is most compact in the [OI] λ6300 line. In [OI] the centroid of the high-velocity gas is typically offset by only 0.2'' from the star whereas in [SII] and [NII] 3 and 3.5 times larger average values have been measured, respectively. In the case of the low-velocity gas, the smallest offset of the emission centroid is also observed in [OI] (typically 0.1'' in [OI] and 0.2'' in [SII]). Our data provide additional support for the model of Kwan & Tademaru (1988, 1995) according to which the HVC observed in the FELs of many TTSs is formed in a well-collimated jet, while the LVC represents gas from a physically distinct flow component (possibly a disk wind or a disk corona). The larger spatial extent of the high-velocity gas in [SII] and [NII] compared to that in [OI] is most probably the result of a jet decreasing in density with increasing distance from the source combined with an increase in excitation. The decrease of the electron density with distance is rather obvious for a jet with diverging stream lines, but why the electron temperature increases is unclear.

Abstract Copyright:

Journal keyword(s): stars: pre-main-sequence - stars: variable - stars: emission-line - ISM: jets and outflows

CDS comments: Table 2: numbering 'NN' (Nos 1-38) in this survey not used in SIMBAD

Simbad objects: 39

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Number of rows : 39

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* V510 Cas Or* 00 12 30.3980375946 +65 33 05.251503588   15.62       K1 16 0
2 V* FM Tau Or* 04 14 13.5839505100 +28 12 49.166941548 14.44   13.80 13.64   M0/2e 196 0
3 V* FN Tau Or* 04 14 14.5943659839 +28 27 58.063377983     14.70 13.68   M5 145 0
4 V* CW Tau Or* 04 14 17.0041128798 +28 10 57.765657757 13.92 13.64 12.36 12.86   K0Ve 324 0
5 V* DD Tau Or* 04 18 31.1271804823 +28 16 29.158626278 15.94 15.49 14.10 13.76   M3.5e+M3.5e 181 0
6 V* CZ Tau Or* 04 18 31.5906879009 +28 16 58.161795569 15.96 16.60 15.70 14.77   M2 131 0
7 V* RY Tau Or* 04 21 57.4132838427 +28 26 35.533990877 10.82 10.34 9.30 9.67 8.87 K1IV/Ve 662 1
8 HD 283572 Or* 04 21 58.8482823933 +28 18 06.511915195   9.80 9.03 9.14   G5IVe 272 0
9 V* T Tau TT* 04 21 59.4323326335 +19 32 06.439974179   11.22 10.12 9.80   K0IV/Ve 1340 1
10 V* FS Tau Or* 04 22 02.1925017485 +26 57 30.331063489 17.57   14.10 15.63   M3.5e+M0e 263 0
11 V* DF Tau Or* 04 27 02.7917481241 +25 42 22.456361256 11.97 12.25 11.42 10.31 9.14 M3Ve 467 1
12 V* DG Tau Or* 04 27 04.6913654419 +26 06 16.041555299 13.57 13.97 10.50 12.28   K6Ve 952 1
13 V* DH Tau Or* 04 29 41.5520056304 +26 32 58.123761109 15.14 14.62 13.10 13.01   M1Ve 276 0
14 V* DK Tau A * 04 30 44.2409691803 +26 01 24.730398215           K5Ve 251 0
15 V* DK Tau Or* 04 30 44.243376 +26 01 24.65328 13.32 14.59 13.05 12.08   K7e+K7e 303 0
16 V* HL Tau Or* 04 31 38.471952 +18 13 58.08504   15.89 14.49 14.39   K5 1254 0
17 IRAS 04287+1807 mul 04 31 38.8 +18 13 57           ~ 796 0
18 V* XZ Tau Or* 04 31 40.0868968022 +18 13 56.642439056     10.40 13.12   M2e+M2e 413 1
19 V* UZ Tau ** 04 32 43.02168 +25 52 30.9036           M4Ve+M1/3Ve 292 0
20 V* GH Tau Or* 04 33 06.2181025969 +24 09 33.628411049     13.20 12.59   M3Ve 172 0
21 V* DL Tau Or* 04 33 39.0766866461 +25 20 38.097973550 14.04 14.59 13.40 11.85 10.89 K7Ve 295 0
22 V* HN Tau Or* 04 33 39.3612389736 +17 51 52.302839814   14.76 13.40 13.05   K5e 226 0
23 V* AA Tau Or* 04 34 55.4222683130 +24 28 53.038273587 13.14 13.34 12.20     K5Ve 649 0
24 V* DO Tau Or* 04 38 28.5882167490 +26 10 49.472067634 12.78 13.44 12.30 13.01   M1Ve 327 1
25 V* DP Tau Or* 04 42 37.6996387891 +25 15 36.992730557 15.84 15.2 13.70 14.42   M0.8 156 1
26 V* DQ Tau Or* 04 46 53.0577037389 +17 00 00.135310040 14.56 13.67 12.00 13.21   M1Ve 300 0
27 V* DR Tau Or* 04 47 06.2152696011 +16 58 42.814250257 12.03 11.86 10.50 12.19   K5Ve 484 0
28 V* UY Aur Or* 04 51 47.3900418279 +30 47 13.552212742 12.82 12.96 11.90 10.59 9.52 M0e+M2.5e 334 0
29 V* RW Aur TT* 05 07 49.5662483 +30 24 05.177426   10.86 9.60 9.95   K1/5e+K5e 729 0
30 V* HS Ori Or* 05 33 01.7601908924 -04 49 18.536447313     16.1     ~ 25 0
31 V* VZ Ori Or* 05 33 45.2606785383 -05 30 49.756973826     13.50   11.77 K1 42 0
32 V* PU Ori Or* 05 36 24.2892555590 -00 42 12.051676633     13.2     ~ 16 0
33 Haro 5-27 Or* 05 39 39.8261219095 -02 31 21.866213622 14.589   14.30 13.92 13.073 K5.5 60 0
34 EM* LkHA 313 TT* 05 47 13.84752 +00 00 17.0532       14.70   M1 16 0
35 V* V697 Mon Or* 06 12 50.3559135709 -06 13 11.486361274   15.60 14.62 14.48   ~ 29 2
36 V* V481 Mon Or* 06 31 09.1394421847 +10 26 10.731485469           K3 13 0
37 V* NX Mon TT* 06 40 41.1407268194 +09 33 57.855783779 15.139 16.43 15.87 15.49 14.401 K7: 69 0
38 EM* AS 353 Or* 19 20 30.9919486938 +11 01 54.604157558   13.22 12.21     K5 184 1
39 V* V536 Aql Or* 19 38 57.413016 +10 30 15.99804     14.85 12.27   KV:e 58 0

    Equat.    Gal    SGal    Ecl

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2021.05.07-16:29:22

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