excitation mechanisms for hot h 2 in the planet-forming regions of protostars
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Excitation Mechanisms for Hot H 2 in the Planet-Forming Regions of Protostars. Mary Barsony (SFSU & SSI), Thomas P. Greene (NASA/ARC), & David A. Weintraub (Vanderbilt U.). - PowerPoint PPT PresentationTRANSCRIPT
Excitation Mechanisms for Hot H2 in the Planet-Forming Regions of ProtostarsMary Barsony (SFSU & SSI), Thomas P. Greene (NASA/ARC), & David A. Weintraub (Vanderbilt U.)
Artist’s rendition of appearance of a typical protostar: bipolar outflow cavity, accretion disk, surrounding infall envelope. Protostars are powerful X-ray sources.
H2 v=1-0 S(1) 2.1218m line spectra. Spectra acquired on 2007 June 24 and 2008 January 24 appear in the left panel, and spectra acquired on 2007 June 25 and 2008 January 25 appear in the right panel.
Quiescent H2 Excitation Mechanisms in Protostars
Scatter Plot of Lx vs H2 v=1-0 S(1) Line Luminosity
Inner Regions of Accretion Disk: The surface layers of the puffed up accretion disk is where the quiescent H2 emission originates.