2014MNRAS.441..964R


Query : 2014MNRAS.441..964R

2014MNRAS.441..964R - Mon. Not. R. Astron. Soc., 441, 964-982 (2014/June-3)

Feedback from winds and supernovae in massive stellar clusters - II. X-ray emission.

ROGERS H. and PITTARD J.M.

Abstract (from CDS):

The X-ray emission from a simulated massive stellar cluster is investigated. The emission is calculated from a 3D hydrodynamical model which incorporates the mechanical feedback from the stellar winds of three O stars embedded in a giant molecular cloud (GMC) clump containing 3240M of molecular material within a 4pc radius. A simple prescription for the evolution of the stars is used, with the first supernova (SN) explosion at t = 4.4Myr. We find that the presence of the GMC clump causes short-lived attenuation effects on the X-ray emission of the cluster. However, once most of the material has been ablated away by the winds, the remaining dense clumps do not have a noticeable effect on the attenuation compared with the assumed interstellar medium (ISM) column. We determine the evolution of the cluster X-ray luminosity, LX, and spectra, and generate synthetic images. The intrinsic X-ray luminosity drops from nearly 1034 erg/s while the winds are `bottled up', to a near-constant value of 1.7x1032 erg/s between t = 1 and 4Myr. LX reduces slightly during each star's red supergiant stage due to the depressurization of the hot gas. However, LX increases to ~ 1034 erg/s during each star's Wolf-Rayet stage. The X-ray luminosity is enhanced by two to three orders of magnitude to ∼ 1037 erg/s for at least 4600yr after each SN explosion, at which time the blast wave leaves the grid and the X-ray luminosity drops. The X-ray luminosity of our simulation is generally considerably fainter than predicted from spherically symmetric bubble models, due to the leakage of hot gas material through gaps in the outer shell. This process reduces the pressure within our simulation and thus the X-ray emission. However, the X-ray luminosities and temperatures which we obtain are comparable to similarly powerful massive young clusters.

Abstract Copyright: © 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society (2014)

Journal keyword(s): hydrodynamics - stars: kinematics and dynamics - stars: massive - X-rays: stars

Simbad objects: 47

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Number of rows : 47
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 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 10264 1
2 SNR B0102-72.3 SNR 01 04 01.2 -72 01 52           ~ 372 1
3 NAME Eridanus Shell sh 02 17 31 +07 49.6           ~ 46 0
4 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 16074 1
5 SNR J052501-693842 SNR 05 25 02.20 -69 38 39.0           ~ 378 1
6 NAME Orion Nebula Cluster OpC 05 35.0 -05 29           ~ 2149 1
7 NAME Trapezium Cluster As* 05 35 16.5 -05 23 14           ~ 1546 1
8 M 42 HII 05 35 17.3 -05 23 28           ~ 3908 0
9 NAME Ori A MoC 05 38 -07.1           ~ 2850 0
10 RMC 136 Cl* 05 38 42.396 -69 06 03.36           ~ 1862 1
11 NAME Horsehead Nebula DNe 05 40 59.0 -02 27 30           ~ 482 0
12 NAME Flame Nebula HII 05 41 42.7 -01 54 44           ~ 695 1
13 NAME Ori B MoC 05 41 43.0 -01 54 44           ~ 1272 0
14 NGC 2024 Cl* 05 41 43 -01 50.5           ~ 1111 1
15 [BCB89] IRS 2b Y*O 05 41 45.490 -01 54 28.78           O8V 44 1
16 HD 46150 Em* 06 31 55.5205071744 +04 56 34.296516096 6.03 6.86 6.73 6.50 6.41 O5V((f))z 382 0
17 HD 46223 Y*O 06 32 09.3068103600 +04 49 24.705695568 6.73 7.50 7.28 6.95 6.79 O4V((f)) 367 0
18 NGC 2244 OpC 06 32 11 +04 54.8           ~ 587 1
19 NAME Rosette Nebula HII 06 32 26.76 +04 47 37.1           ~ 469 1
20 NAME Rosette Molecular Cloud MoC 06 34.7 +04 02           ~ 246 0
21 NAME Pup A SNR 08 24 07 -42 59.8           ~ 557 1
22 RCW 38 SFR 08 59 05.50 -47 30 39.4           ~ 291 2
23 [FP74] RCW 38 IRS 2 Y*O 08 59 05.6555109888 -47 30 40.941723780       14.05 11.20 O5.5V 23 1
24 V* V712 Car EB* 10 23 58.0126366512 -57 45 48.937268268 15.466 15.473 13.5 12.6   O3If*/WN6+O3If*/WN6 158 1
25 Cl Westerlund 2 OpC 10 23 58.1 -57 45 49           ~ 314 0
26 GUM 29 HII 10 24 14.6 -57 46 58           ~ 198 0
27 WR 20b WR* 10 24 18.3978418584 -57 48 29.776921704     13.7 12.0   WN6ha 53 0
28 Cl Trumpler 16 OpC 10 45 01 -59 42.0   5.35 5.0     ~ 454 0
29 NGC 3372 HII 10 45 02.23 -59 41 59.8           ~ 948 2
30 HD 97319 Y*O 11 11 06.1590329208 -61 07 04.550758320 8.08 8.71 8.51 9.28   O7.5IV((f)) 63 0
31 NGC 3576 HII 11 11 49.8 -61 18 14           ~ 232 2
32 V* EM Car EB* 11 12 04.5060592584 -61 05 42.944560584 8.06 8.80 8.54 9.25   O7.5V((f))+O7.5V((f)) 156 0
33 RCW 57 HII 11 14.7 -61 12           ~ 14 0
34 HD 97950 Cl* 11 15 07.346 -61 15 38.52 9.64 9.83 9.03 9.69   ~ 187 2
35 NGC 3603 OpC 11 15 11 -61 15.5           ~ 1013 1
36 SNR G292.0+01.8 SNR 11 24 59 -59 19.1           ~ 307 1
37 Cl Westerlund 1 OpC 16 47 04.00 -45 51 04.9           ~ 510 0
38 NGC 6334 HII 17 20 51 -36 06.9           ~ 639 0
39 NAME Galactic Center reg 17 45 39.60213 -29 00 22.0000           ~ 13004 0
40 NAME Arches Cluster Cl* 17 45 50.5 -28 49 28           ~ 687 0
41 NAME Quintuplet Cluster OpC 17 46 13.9 -28 49 48           ~ 493 0
42 M 8 HII 18 03 37 -24 23.2           ~ 583 1
43 NAME Her 36SE SB* 18 03 40.3201232304 -24 22 42.857540472 10.26 11.022 10.372 10.267   O7:V 185 0
44 NAME Hourglass Nebula ISM 18 03 41.1 -24 22 37           ~ 75 2
45 NGC 6530 OpC 18 04 31 -24 21.5           ~ 382 0
46 NGC 6618 OpC 18 20 47 -16 10.3           ~ 1546 0
47 OHIO N 002 Rad 20 21 +37.5           ~ 13 1

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2022.07.06-09:47:53

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