J/ApJ/921/91 Catastrophic cooling in superwinds. II. (Danehkar+, 2021)
Catastrophic cooling in superwinds. II. Exploring the parameter space.
Danehkar A., Oey M.S., Gray W.J.
<Astrophys. J. 921, 91 (2021)>
=2021ApJ...921...91D 2021ApJ...921...91D (SIMBAD/NED BibCode)
ADC_Keywords: H II regions ; Galaxies, peculiar ; Abundances
Keywords: superbubbles - superclusters - cooling flows - star forming regions -
H II regions - starburst galaxies - emission line galaxies -
Lyman-break galaxies - Lyman-alpha galaxies
Abstract:
Superwinds and superbubbles driven by mechanical feedback from super
star clusters (SSCs) are common features in many star-forming
galaxies. While the adiabatic fluid model can well describe the
dynamics of superwinds, several observations of starburst galaxies
revealed the presence of compact regions with suppressed superwinds
and strongly radiative cooling, i.e., catastrophic cooling. In the
present study, we employ the non-equilibrium atomic chemistry and
cooling package MAIHEM, built on the FLASH hydrodynamics code, to
generate a grid of models investigating the dependence of cooling
modes on the metallicity, SSC outflow parameters, and ambient density.
While gas metallicity plays a substantial role, catastrophic cooling
is more sensitive to high mass-loading and reduced kinetic heating
efficiency. Our hydrodynamic simulations indicate that the presence of
a hot superbubble does not necessarily imply an adiabatic outflow, and
vice versa. Using CLOUDY photoionization models, we predict UV and
optical line emission for both adiabatic and catastrophic cooling
outflows, for radiation-bounded and partially density-bounded models.
Although the line ratios predicted by our radiation-bounded models
agree well with observations of star-forming galaxies, they do not
provide diagnostics that unambiguously distinguish the parameter space
of catastrophically cooling flows. Comparison with observations
suggests the possibility of minor density bounding, non-equilibrium
ionization, and/or observational bias toward the central outflow
regions.
Description:
Table 3 presents integrated luminosities from the different
photoionization models.
Each file is named as [case]-[bound].dat e.g. cpi-radi.dat,
where [case] is for the ionization case, pi: photoionization
equilibrium (PIE) and cpi: collisional ionization + photoionization
equilibrium (CIE+PIE), and [bound] for the optical depth model, radi:
fully radiation-bounded, pden: partially density-bounded, and dens:
fully density-bounded.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
pi-radi.dat 1290 132 Fully radiation-bounded PIE
pi-pden.dat 1290 132 Partially density-bounded PIE
pi-dens.dat 1290 132 Fully density-bounded PIE
cpi-radi.dat 1290 132 Fully radiation-bounded CIE+PIE
cpi-pden.dat 1290 132 Partially density-bounded CIE+PIE
cpi-dens.dat 1290 132 Fully density-bounded CIE+PIE
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Byte-by-byte Description of file: pi-*.dat cpi-*.dat
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Bytes Format Units Label Explanations
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1- 6 F6.4 Sun metal Metallicity (in Zsun unit)
8- 16 F9.7 Msun/yr dM/dt Mass-loss rate
18- 23 F6.1 km/s Vinf Wind terminal speed
25- 27 F3.1 pc Rsc Cluster radius
29- 36 E8.3 yr age Cluster current age
38- 45 E8.3 Msun Mstar Cluster total stellar mass
47- 51 F5.2 [10-7W] logLion Logarithmic ionizing
53- 58 F6.1 cm-3 Namb Ambient density
60- 66 F7.1 K Tamb Ambient temperature from Cloudy
68- 73 F6.1 pc Rmax Maximum radius
75- 80 F6.1 pc Raper Aperture radius
82- 86 F5.1 pc Rshell Shell outer radius
88- 93 F6.1 pc Rstr Stromgren radius from Cloudy
95- 99 F5.1 pc Rbin Bubble inner radius
101- 105 F5.1 pc Rbout Bubble outer radius
107- 114 E8.3 K Tbubble Median bubble temperature
116- 123 E8.3 K Tadi Median temperature of adiabatic
125- 132 E8.3 K Twind Median temperature of radiative
134- 138 F5.2 --- logUsp Ioniz.param. log(Usp) from Cloudy
140 I1 --- thin [0/1] Optically thin (1) and thick (0)
142 I1 --- mode [1/6] Wind mode (1)
144- 156 E13.8 10-7W H1-1216 Luminosity of Lyα 1216
emission line
158- 170 E13.8 10-7W H1-6563 Luminosity of Hα 6563
emission line
172- 184 E13.8 10-7W H1-4861 Luminosity of Hβ 48611
emission line
186- 198 E13.8 10-7W He1-5876 Luminosity of HeI 5876 emission line
200- 212 E13.8 10-7W He1-6678 Luminosity of HeI 6678 emission line
214- 226 E13.8 10-7W He1-7065 Luminosity of HeI 7065 emission line
228- 240 E13.8 10-7W He2-1640 Luminosity of HeII 1640 emission line
242- 254 E13.8 10-7W He2-4686 Luminosity of HeII 4686 emission line
256- 268 E13.8 10-7W C2-1335 Luminosity of CII 1335 emission line
270- 282 E13.8 10-7W C2-2326-blnd Luminosity of CII 2326 blended
emission line
284- 296 E13.8 10-7W C3-977 Luminosity of CIII 977 emission line
298- 310 E13.8 10-7W C3-1909-blnd Luminosity of CIII] 1909 blended
emission line
312- 324 E13.8 10-7W C3-1907 Luminosity of CIII] 1907 emission line
326- 338 E13.8 10-7W C3-1908 Luminosity of CIII] 1908 emission line
340- 352 E13.8 10-7W C3-1549 Luminosity of CIII 1549 emission line
354- 366 E13.8 10-7W C4-1549-blnd Luminosity of CIV 1549 blended
emission line
368- 380 E13.8 10-7W C4-1548 Luminosity of CIV 1548 emission line
382- 394 E13.8 10-7W C4-1551 Luminosity of CIV 1551 emission line
396- 408 E13.8 10-7W N1-5200 Luminosity of [NI] 5200 emission line
410- 422 E13.8 10-7W N2-5755 Luminosity of [NII] 5755 emission line
424- 436 E13.8 10-7W N2-6548 Luminosity of [NII] 6548 emission line
438- 450 E13.8 10-7W N2-6583 Luminosity of [NII] 6583 emission line
452- 464 E13.8 10-7W N3-1750 Luminosity of NIII 1750 emission line
466- 478 E13.8 10-7W N3-1750-blnd Luminosity of NIII 1750 blended
emission line
480- 492 E13.8 10-7W N3-991 Luminosity of NIII 991 emission line
494- 506 E13.8 10-7W N4-1483 Luminosity of NIV 1483 emission line
508- 520 E13.8 10-7W N4-1487 Luminosity of NIV 1487 emission line
522- 534 E13.8 10-7W N4-1486-blnd Luminosity of NIV 1486 blended
emission line
536- 548 E13.8 10-7W N5-1239 Luminosity of NV 1239 emission line
550- 562 E13.8 10-7W N5-1243 Luminosity of NV 1243 emission line
564- 576 E13.8 10-7W N5-1240-blnd Luminosity of NV 1240 blended
emission line
578- 590 E13.8 10-7W O1-1304-blnd Luminosity of OI 1304 blended
emission line
592- 604 E13.8 10-7W O1-6300 Luminosity of [OI] 6300 emission line
606- 618 E13.8 10-7W O1-6364 Luminosity of [OI] 6364 emission line
620- 632 E13.8 10-7W O2-3726 Luminosity of [OII] 3726 emission line
634- 646 E13.8 10-7W O2-3729 Luminosity of [OII] 3729 emission line
648- 660 E13.8 10-7W O2-7319 Luminosity of [OII] 7319 emission line
662- 674 E13.8 10-7W O2-7320 Luminosity of [OII] 7320 emission line
676- 688 E13.8 10-7W O2-7323-blnd Luminosity of [OII] 7323 blended
emission line
690- 702 E13.8 10-7W O2-7330 Luminosity of [OII] 7330 emission line
704- 716 E13.8 10-7W O2-7331 Luminosity of [OII] 7331 emission line
718- 730 E13.8 10-7W O2-7332-blnd Luminosity of [OII] 7332 blended
emission line
732- 744 E13.8 10-7W O3-1661 Luminosity of OIII] 1661 emission line
746- 758 E13.8 10-7W O3-1666 Luminosity of OIII] 1666 emission line
760- 772 E13.8 10-7W O3-2321 Luminosity of [OIII] 2321 emission line
774- 786 E13.8 10-7W O3-4363 Luminosity of [OIII] 4363 emission line
788- 800 E13.8 10-7W O3-4959 Luminosity of [OIII] 4959 emission line
802- 814 E13.8 10-7W O3-5007 Luminosity of [OIII] 5007 emission line
816- 828 E13.8 10-7W O4-1402-blnd Luminosity of OIV 1402 blended
emission line
830- 842 E13.8 10-7W O6-1035-blnd Luminosity of OVI 1035 blended
emission line
844- 856 E13.8 10-7W O6-1032 Luminosity of OVI 1032 emission line
858- 870 E13.8 10-7W O6-1038 Luminosity of OVI 1038 emission line
872- 884 E13.8 10-7W Ne3-1815 Luminosity of NeIII 1815 emission line
886- 898 E13.8 10-7W Ne3-3342 Luminosity of [NeIII] 3342 emission line
900- 912 E13.8 10-7W Ne3-3869 Luminosity of [NeIII] 3869 emission line
914- 926 E13.8 10-7W Ne3-3967 Luminosity of [NeIII] 3967 emission line
928- 940 E13.8 10-7W Ne4-2424-blnd Luminosity of NeIV 2424 blended
emission line
942- 954 E13.8 10-7W Ne5-3426 Luminosity of NeV 3426 emission line
956- 968 E13.8 10-7W Si2-1190 Luminosity of SiII 1190 emission line
970- 982 E13.8 10-7W Si2-1193 Luminosity of SiII 1193 emission line
984- 996 E13.8 10-7W Si2-1265 Luminosity of SiII 1265 emission line
998-1010 E13.8 10-7W Si2-1304 Luminosity of SiII 1304 emission line
1012-1024 E13.8 10-7W Si2-1309 Luminosity of SiII 1309 emission line
1026-1038 E13.8 10-7W Si2-1533 Luminosity of SiII 1533 emission line
1040-1052 E13.8 10-7W Si2-1817 Luminosity of SiII 1817 emission line
1054-1066 E13.8 10-7W Si3-1207 Luminosity of SiIII 1207 emission line
1068-1080 E13.8 10-7W Si3-1883 Luminosity of SiIII 1883 emission line
1082-1094 E13.8 10-7W Si3-1892 Luminosity of SiIII 1892 emission line
1096-1108 E13.8 10-7W Si3-1888-blnd Luminosity of SiIII 1888 blended
emission line
1110-1122 E13.8 10-7W Si4-1394 Luminosity of SiIV 1394 emission line
1124-1136 E13.8 10-7W Si4-1403 Luminosity of SiIV 1403 emission line
1138-1150 E13.8 10-7W S2-4069 Luminosity of [SII] 4069 emission line
1152-1164 E13.8 10-7W S2-4076 Luminosity of [SII] 4076 emission line
1166-1178 E13.8 10-7W S2-6716 Luminosity of [SII] 6716 emission line
1180-1192 E13.8 10-7W S2-6731 Luminosity of [SII] 6731 emission line
1194-1206 E13.8 10-7W S3-9069 Luminosity of [SIII] 9069 emission line
1208-1220 E13.8 10-7W S3-9531 Luminosity of [SIII] 9531 emission line
1222-1234 E13.8 10-7W Ar3-7136 Luminosity of [ArIII] 7136 emission line
1236-1248 E13.8 10-7W Ar3-7751 Luminosity of [ArIII] 7751 emission line
1250-1262 E13.8 10-7W Ar4-4711 Luminosity of [ArIV] 4711 emission line
1264-1276 E13.8 10-7W Ar4-4740 Luminosity of [ArIV] 4740 emission line
1278-1290 E13.8 10-7W Ar5-7006 Luminosity of [ArV] 7006 emission line
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Note (1): Wind mode as follows:
1 = AW: adiabatic wind
2 = AB: adiabatic bubble
3 = AP: adiabatic, pressure-confined
4 = CC: catastrophic cooling
5 = CB: catastrophic cooling bubble
6 = CP: catastrophic cooling, pressure-confined
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Acknowledgements:
Ashkbiz Danehkar, ashkbiz.danehkar(at)gmail.com
References:
Gray et al., Paper I 2019ApJ...887..161G 2019ApJ...887..161G
(End) Ashkbiz Danehkar [Michigan, USA], Patricia Vannier [CDS] 11-Nov-2021