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Work: State-resolved rotational cross sections and thermal rate coefficients for <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" altimg="si24.gif" display="inline" overflow="scroll"><mml:mrow><mml:mi mathvariant="italic">ortho</mml:mi><mml:mtext>-</mml:mtext><mml:mo>/</mml:mo><mml:mi mathvariant="italic">para</mml:mi><mml:mtext>-</mml:mtext><mml:msub><mml:mrow><mml:mtext>H</mml:mtext></mml:mrow><mml:mrow><mml:mn>2</mml:mn></mml:mrow></mml:msub><mml:mo>+</mml:mo><mml:mtext>HD</mml:mtext></mml:mrow></mml:math> at low temperatures and HD + HD elastic scattering
The Formation of the First Stars. I. The Primordial Star‐forming Cloud
Volker Bromm, P. Coppi, Richard B. Larson
Article20023 citationsABI