scholarly journals Fragmentation inside atomic cooling haloes exposed to Lyman–Werner radiation

2018 ◽  
Vol 475 (4) ◽  
pp. 4636-4647 ◽  
Author(s):  
John A Regan ◽  
Turlough P Downes
Keyword(s):  
Atomic Cooling

scholarly journals A laser diode system for 40K-87Rb atomic cooling

2006 ◽  
Vol 55 (12) ◽  
pp. 6342
Author(s):  
Wei Dong ◽  
Chen Hai-Xia ◽  
Xiong De-Zhi ◽  
Zhang Jing
Keyword(s):  
Laser Diode ◽  
Atomic Cooling ◽  
Diode System

scholarly journals The origin of spin in galaxies: clues from simulations of atomic cooling haloes

2015 ◽  
Vol 452 (1) ◽  
pp. 784-802 ◽  
Author(s):  
Joaquin Prieto ◽  
Raul Jimenez ◽  
Zoltán Haiman ◽  
Roberto E. González
Keyword(s):  
Atomic Cooling

Adiabatic atomic cooling in cavity QED

2007 ◽  
pp. 185-194
Author(s):  
T. Zaugg ◽  
G. Lenz ◽  
P. Meystre
Keyword(s):  
Cavity Qed ◽  
Atomic Cooling

scholarly journals IRAS Observations of Collisionally Heated Dust in Large Magellanic Cloud Supernova Remnants

1988 ◽  
Vol 101 ◽  
pp. 383-386
Author(s):  
James R. Graham ◽  
A. Evans ◽  
J.S. Albinson ◽  
M.F. Bode ◽  
W.P.S. Meikle
Keyword(s):  
Interstellar Medium ◽  
Supernova Remnants ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Substantial Fraction ◽  
X Ray ◽  
Ir Sources ◽  
Atomic Cooling ◽  
Dust Grain ◽  
Ir Emission

AbstractIRAS additional observations show that luminous (104−105 L⊙) far-IR sources are associated with the Large Magellanic Cloud (LMC) supernova remnants N63A, N49, N49B, and N186D. Comparison of the IRAS and X-ray data shows that a substantial fraction of the IR emission from three of the SNRs can be accounted for by collisionally heated dust. The ratio of dust-grain cooling to total atomic cooling is ~10 in X-ray emitting gas (T~106 K). We show why dust cooling does not dominate, but probably speeds SNR evolution in an inhomogeneous interstellar medium.

scholarly journals Atomic cooling via AC Stark shift

2014 ◽  
Vol 39 (3) ◽  
pp. 536 ◽  
Author(s):  
Jennifer A. Black ◽  
Holger Schmidt
Keyword(s):  
Stark Shift ◽  
Atomic Cooling

scholarly journals The emergence of the first star-free atomic cooling haloes in the Universe

2020 ◽  
Vol 492 (2) ◽  
pp. 3021-3031 ◽  
Author(s):  
John A Regan ◽  
John H Wise ◽  
Brian W O’Shea ◽  
Michael L Norman
Keyword(s):  
Black Hole ◽  
Early Universe ◽  
Metal Enrichment ◽  
Massive Black Hole ◽  
Metal Free ◽  
Physical Conditions ◽  
Radiation Fields ◽  
Atomic Cooling ◽  
The Universe ◽  
Massive Galaxy

ABSTRACT Using the Renaissance suite of simulations, we examine the emergence of pristine atomic cooling haloes that are both metal free and star free in the early universe. The absence of metals prevents catastrophic cooling, suppresses fragmentation, and may allow for the formation of massive black hole seeds. Here we report on the abundance of pristine atomic cooling haloes found and on the specific physical conditions that allow for the formation of these direct-collapse-black hole (DCBH) haloes. In total, in our simulations we find that 79 DCBH haloes form before a redshift of 11.6. We find that the formation of pristine atomic haloes is driven by the rapid assembly of the atomic cooling haloes with mergers, both minor and/or major, prior to reaching the atomic cooling limit a requirement. However, the ability of assembling haloes to remain free of (external) metal enrichment is equally important and underlines the necessity of following the transport of metals in such simulations. The candidate DCBH-hosting haloes we find have been exposed to mean Lyman–Werner radiation fields of J21 ∼1 and typically lie at least 10 kpc (physical) from the nearest massive galaxy. The growth rates of the haloes reach values of greater than 107$\rm {M_{\odot }}~$ per unit redshift, leading to significant dynamical heating and the suppression of efficient cooling until the halo crosses the atomic cooling threshold. Finally, we also find five synchronized halo candidates where pairs of pristine atomic cooling haloes emerge that are both spatially and temporally synchronized.

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