2001ApJ...546..299B


Query : 2001ApJ...546..299B

2001ApJ...546..299B - Astrophys. J., 546, 299-323 (2001/January-1)

Irradiated Herbig-Haro jets in the Orion nebula and near NGC 1333.

BALLY J. and REIPURTH B.

Abstract (from CDS):

We report the discovery of a dozen Herbig-Haro jets illuminated by the Lyman continuum (λ<912 Å) and/or softer far-ultraviolet (912<λ<2000 Å) radiation fields of nearby high-mass stars. Five irradiated outflows lie in the outer parts of the Orion Nebula (HH 502-506), and seven lie near the reflection nebula NGC 1333 in the Perseus molecular cloud (HH 333-336 and HH 497-499). These stellar outflows are powered by optically visible low-mass young stars that suffer relatively low extinction and seem not to be embedded within opaque cloud cores. We propose that the UV radiation field has eroded residual material left over from their formation on a timescale short compared to the ages of these star-forming regions. Many of the irradiated jets exhibit unusual C-shaped symmetry. In the outskirts of the Orion Nebula, most irradiated jets appear to bend away from the core of the nebula. On the other hand, in NGC 1333, the C-shaped jets tend to bend back toward the cluster center. Jet bending in the Orion Nebula may be dominated by either the outflow of material from the nebular core or by the rocket effect pushing on the irradiated portion of a mostly neutral jet beam. But in NGC 1333, jet bending may indicate that the source stars have been ejected from the cluster core. Many irradiated jets are asymmetric with one beam much brighter than the other. When fully photoionized, irradiated jets may provide unique insights into the physical conditions within outflows powered by young stars, permitting the determination of the density and location of stellar ejecta even in the absence of shocks. We present a model for the photoionization of these outflows by external radiation fields and discuss possible mechanisms for producing the observed asymmetries. In particular, we demonstrate that the UV radiation field may alter the amount of cloud material entrained by the jet. Radiation-induced variations in mass loading and beam heating can produce differences in the beam velocities and spreading rates, which in turn determine the surface brightness of the radiating plasma. In a bipolar irradiated jet in which both beams have the same mass-loss rate and opening angle, the slower beam will appear brighter at a given distance from the source. On the other hand, if both beams spread orthogonal to the jet propagation direction with the same speed (e.g., both beams have the same internal sound speed or shocks with similar physical conditions), the faster beam will appear brighter at the same distance from the source. Thus, depending on the parameters, either the faster or slower beam of a jet can be brighter. Finally, we report the discovery of some large-scale bow shocks that face the core of the Orion Nebula and surround visible young stars. These wind-wind collision fronts provide further evidence for a large-scale mass flow originating near the nebular core.

Abstract Copyright:

Journal keyword(s): ISM: Herbig-Haro Objects - ISM: Individual: NGC Number: NGC 1333 - ISM: Individual: Name: Orion Nebula - ISM: Jets and Outflows - Stars: Formation - Stars: Pre-Main-Sequence

Nomenclature: Table 2: HH NNNWN N=55, HH NNNWWN N=11. Table 2:[BR2001] HH NNN jet N=7, [BR2001] HH NNN W jet N=2, [BR2001] HH 502 N3 wing N=1, [BR2001] HH 504 bow N=1, [BR2001] HH NNN star N=13. Fig.2: [BR2001] HH 502 star A (Nos A-C). Table 5: [BR2001] LLN (Nos LL1 to LL7). Table 6: [BR2001] HH CN (Nos C1-C3).

Status at CDS : All or part of tables of objects will not be ingested in SIMBAD.

Simbad objects: 92

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Number of rows : 92
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 HH 547 HH 03 27 54.5 +31 09 36           ~ 1 0
2 HH 339 HH 03 28 30.9 +31 14 46           ~ 8 1
3 HH 542 HH 03 28 49.5 +31 18 47           ~ 1 0
4 HH 334 HH 03 28 51.7 +31 22 38           ~ 8 0
5 HH 498 HH 03 28 52.2 +31 22 45           ~ 5 0
6 HH 12 HH 03 28 59.4 +31 20 11           ~ 119 1
7 HH 344 HH 03 29 01.7 +31 13 16           ~ 7 0
8 HH 333W4 HH 03 29 02.4 +31 25 46           ~ 2 0
9 HH 333W3 HH 03 29 03.6 +31 25 46           ~ 2 0
10 NAME HH 7-11 FIR 03 29 03.9 +31 16 06           ~ 346 0
11 HH 333W2 HH 03 29 06.2 +31 25 50           ~ 2 0
12 HH 333W1 HH 03 29 10.9 +31 26 03           ~ 2 0
13 HH 6 HH 03 29 11.2 +31 18 34           ~ 64 0
14 NGC 1333 OpC 03 29 11 +31 18.6           ~ 1345 1
15 2MASS J03291177+3126095 Y*O 03 29 11.7737851008 +31 26 09.328679592           ~ 23 0
16 HH 544 HH 03 29 14.3 +31 22 47           ~ 1 0
17 HH 543 HH 03 29 14.7 +31 27 21           ~ 1 0
18 HH 345 HH 03 29 15.1 +31 13 26           ~ 6 0
19 HH 347 HH 03 29 15.7 +31 15 22           ~ 8 0
20 EM* LkHA 270 TT* 03 29 17.6758022904 +31 22 44.892332544   16.344 14.639 13.994   K2/3IIIe 80 0
21 HH 335 HH 03 29 17.7 +31 23 03           ~ 9 0
22 BD+30 549 Y*O 03 29 19.7773614209 +31 24 57.044926178 10.81 10.95 10.47 10.587   B8/9V 102 0
23 HH 5 HH 03 29 20.424 +31 12 51.28           ~ 41 1
24 HH 17 Y*O 03 29 20.4245077872 +31 18 34.234290072     16.38     K6.0 53 0
25 HH 346 HH 03 29 21.6 +31 15 28           ~ 4 0
26 ASR 79 Y*O 03 29 24.0886223107 +31 19 57.383186997           M2.5V 49 0
27 HH 348 HH 03 29 25.4 +31 13 34           ~ 7 0
28 HH 496 HH 03 29 34.7 +31 24 22           ~ 2 0
29 HH 349 HH 03 29 36.2 +31 13 33           ~ 5 0
30 HH 336 * 03 29 39.77 +31 17 44.0           ~ 8 0
31 HH 545 HH 03 29 52.4 +31 24 31           ~ 1 0
32 HH 546 HH 03 29 58.4 +31 13 59           ~ 1 0
33 HH 505N3 HH 05 34 39.4 -05 22 04           ~ 3 0
34 HH 505N2 HH 05 34 39.6 -05 22 07           ~ 4 0
35 HH 505 HH 05 34 40.8 -05 22 39           ~ 14 1
36 HH 505N1 HH 05 34 40.8 -05 22 35           ~ 4 0
37 [BR2001] LL2 of? 05 34 40.9 -05 22 42           ~ 2 1
38 HH 503W2 HH 05 34 43.6 -05 31 28           ~ 2 0
39 HH 503W1 HH 05 34 44.8 -05 31 32           ~ 2 0
40 HH 503 HH 05 34 48.4 -05 31 43           ~ 3 0
41 HH 503E1 HH 05 34 51.6 -05 32 13           ~ 2 0
42 HH 503E2 HH 05 34 55 -05 33.1           ~ 2 0
43 HH 537 HH 05 35 01.3 -05 14 07           ~ 1 0
44 HH 504N2 HH 05 35 02.8 -05 28 55           ~ 2 0
45 HH 504N1 HH 05 35 03.0 -05 29 00           ~ 2 0
46 HH 504 HH 05 35 03.5 -05 29 22           ~ 4 0
47 [BR2001] LL1 of? 05 35 05.580 -05 25 19.47           ~ 2 1
48 V* LL Ori Or* 05 35 05.6361678504 -05 25 19.520320800 12.997 12.309 11.517   10.034 K0-K3e 104 1
49 HH 541 HH 05 35 06.0 -05 33 30           ~ 2 0
50 HH 269 HH 05 35 09.1 -05 23 44           ~ 41 0
51 HH 202 HH 05 35 11.5 -05 22 46           ~ 70 4
52 HH 201 HH 05 35 11.5 -05 21 54           ~ 38 2
53 HH 205 HH 05 35 11.703 -05 20 24.69           ~ 33 0
54 HH 206 HH 05 35 12.5 -05 20 38           ~ 22 0
55 HH 207 HH 05 35 12.7 -05 20 49           ~ 29 0
56 HH 208A HH 05 35 13.8 -05 22 22           ~ 22 0
57 HH 209 HH 05 35 13.9 -05 21 47           ~ 20 0
58 [LB2000] 154-041 * 05 35 15.45928 -05 20 40.6911           ~ 52 0
59 HH 44 HH 05 35 16.2 -05 10 26           ~ 8 0
60 * tet01 Ori C SB* 05 35 16.4662967280 -05 23 22.921811880 4.20 5.15 5.13 4.91 4.73 O7Vp 1352 1
61 NAME Trapezium Cluster As* 05 35 16.5 -05 23 14           ~ 1558 1
62 M 42 HII 05 35 17.3 -05 23 28           ~ 3937 0
63 HH 540 HH 05 35.3 -05 31           ~ 9 0
64 HH 536 HH 05 35 18.4 -05 12 45           ~ 2 0
65 HH 535 HH 05 35 19.08 -05 11 41.3           ~ 2 0
66 HH 203 HH 05 35 22.2 -05 24 58           ~ 70 4
67 HH 204 HH 05 35 22.6 -05 25 13           ~ 75 4
68 HH 502S8 HH 05 35 25.1 -05 31 39           ~ 3 0
69 HH 384 HH 05 35 25.4 -05 09 23           ~ 4 1
70 HH 502S7 HH 05 35 26.0 -05 30 54           ~ 5 0
71 HH 502S6 HH 05 35 26.1 -05 30 39           ~ 4 0
72 HH 502S5 HH 05 35 26.6 -05 30 17           ~ 4 0
73 HH 502S4 HH 05 35 27.0 -05 30 04           ~ 4 0
74 OMC 2 MoC 05 35 27 -05 10.1           ~ 433 1
75 HH 502S3 HH 05 35 27.1 -05 29 59           ~ 3 0
76 HH 502S2 HH 05 35 27.2 -05 29 53           ~ 3 0
77 HH 502S1 HH 05 35 27.5 -05 29 45           ~ 4 0
78 HH 502 HH 05 35 27.9 -05 29 35           ~ 10 0
79 HH 502N1 HH 05 35 28.1 -05 29 28           ~ 3 0
80 HH 533 HH 05 35 29.5 -05 10 01           ~ 2 0
81 HH 502N2 HH 05 35 30.1 -05 28 55           ~ 5 0
82 HH 502N3 HH 05 35 30.8 -05 28 43           ~ 5 0
83 M 43 HII 05 35 31 -05 16.2           ~ 180 0
84 HH 538 HH 05 35 33.3 -05 13 09           ~ 1 0
85 HH 400 HH 05 35 34 -05 30.5           ~ 9 0
86 HH 539 HH 05 35 37.0 -05 11 43           ~ 1 0
87 HH 532 HH 05 35 46.1 -05 09 53           ~ 1 0
88 * nu. Ori SB* 06 07 34.3258759 +14 46 06.506096 3.6 4.240 4.397     B3IV 226 0
89 HH 506 HH ~ ~           ~ 2 0
90 HH 495 HH ~ ~           ~ 2 0
91 HH 499 HH ~ ~           ~ 5 0
92 HH 497 HH ~ ~           ~ 3 0

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2022.10.03-17:01:18

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