High Resolution Near-Infrared Spectroscopy of Cool Dwarf Stars. (arXiv:1811.05572v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Dupree_A/0/1/0/all/0/1">Andrea Dupree</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Brickhouse_N/0/1/0/all/0/1">Nancy Brickhouse</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Irwin_J/0/1/0/all/0/1">Jonathan Irwin</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Kurucz_R/0/1/0/all/0/1">Robert Kurucz</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Newton_E/0/1/0/all/0/1">Elisabeth Newton</a> (2) ((1) Center for Astrophysics | Harvard &amp; Smithsonian, Cambridge, MA USA (2) Massachusetts Institute of Technology, Cambridge, MA USA, and Dartmouth College, Hanover, NH USA)

We present results from a near infrared survey of the He I line (10830
Angstrom) in cool dwarf stars taken with the PHOENIX spectrograph at the 4-m
Mayall telescope at Kitt Peak National Observatory. Spectral synthesis of this
region reproduces some but not all atomic and molecular features. The
equivalent width of the He line appears directly correlated with the soft X-ray
stellar surface flux except among the coolest M dwarf stars, where the helium
is surprisingly weak.

We present results from a near infrared survey of the He I line (10830
Angstrom) in cool dwarf stars taken with the PHOENIX spectrograph at the 4-m
Mayall telescope at Kitt Peak National Observatory. Spectral synthesis of this
region reproduces some but not all atomic and molecular features. The
equivalent width of the He line appears directly correlated with the soft X-ray
stellar surface flux except among the coolest M dwarf stars, where the helium
is surprisingly weak.

http://arxiv.org/icons/sfx.gif