Abstract
The enhancement of the rate coefficient for the radiative association of He and H+ to form HeH+ arising from stimulated emission due to a blackbody radiation field is calculated. The effects on the fractional abundance of HeH+ in the early universe, in supernova ejecta, and in planetary nebulae are small. There may occur some enhancement in the abundance of HeH+ in quasar broad-line clouds.
Highlights
Processes that lead to the formation and destruction of ejecta, planetary nebulae, and quasars
In this paper we extend the theory of radiative association to include stimulated emission and calculate rate coefÐcients for the formation of HeHas a function of the mploeanrtagtt-eulrivreetdeT,mr.ipnSevpreaertcsueiarlepraetTdtmeisnstaoioncndiatiisbolngaicvrkeebnsootdnoyanthcreeasdtir(aDetaiaotbmnreontwetsmok-fi & Herzberg 1978 ; Roberge & Dalgarno 1982) seen in this isantabTwtoehuh,eniDcdh(sRpsVto)aXnits(teRatehn)ieegisoernauthdsso,eialdupl itoepiloteoenclnetwtr-iiaaicltllhdoeiwenpieeogrdelgen,yvmtarcoaluumnrevseiEetnintofJ,on.arntrdhaet/eJnX(fR1ro&) mis quantum state o aT to o bT is given by the Fermi Golden Rule expression (Schi† 1968)
We explore the possibility for enhancement of the rate of formation for HeHin the early universe when stimulated by the cosmic background radiation (CBR) radiation Ðeld
Summary
Processes that lead to the formation and destruction of ejecta, planetary nebulae, and quasars. Atomic units are used throughout, unless stated otherwise. The molecular ion HeHin astrophysical environments have been the subject of a number of investigations
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