The Search for H- in Astrophysical Environments

Details The Search for H- in Astrophysical Environments The Search for H- in Astrophysical Environments

Sep 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008apj...684..358r&link_type=abstract

The Astrophysical Journal, Volume 684, Issue 1, pp. 358-363.

Astronomy and Astrophysics

Astronomy

7

Ism: Abundances, Ism: Atoms, Ism: Lines And Bands, Ism: Planetary Nebulae: General

Scientific paper

The negative ion H- is widely understood to be important in many astrophysical environments, including the atmospheres of late-type stars like the Sun. However, the ion has never been detected spectroscopically outside the laboratory. A search for the far-ultraviolet autodetaching transitions of H- in interstellar and circumstellar matter seems to be the best hope for directly detecting this ion. We undertook a highly sensitive search using data from the FUSE instrument. We concentrated on two types of sight lines: planetary nebulae, where model calculations suggest a sufficient abundance of H- to be determined, and translucent clouds, where H- might form on dust grains as an intermediate step in molecular hydrogen formation. Upper limits on H- abundances were set.

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