Query : 1998A&A...336..613S

1998A&A...336..613S - Astronomy and Astrophysics, volume 336, 613-625 (1998/8-2)

Chromospheric modelling of the Hα and NaI D lines in five M dwarfs of low to high activity level.


Abstract (from CDS):

We have obtained simultaneous high resolution Hα and NaI D spectra of five dwarf M stars that span a wide range in chromospheric activity level. The observed NaI D lines exhibit behavior that is qualitatively similar to that of more well established diagnostics such as the CaII HK lines: as the activity level, as indicated by the Hα line, increases, the absorption core brightens and then develops an emission reversal. We compare the observed profiles with computed non-LTE profiles from a grid of chromospheric/transition region models. We find that the Hα and NaI D lines tend to be in general agreement as indicators of approximate chromospheric activity level. However, the Hα line systematically indicates a value for the mass loading at the onset of the Transition Region and the location of Tmin that is 0.4 dex lower in column mass density than that indicated by NaI D. Therefore, the profile of both lines cannot be simultaneously well fit for all but one of our stars. We also find, in agreement with the pioneering study of Andretta et al. (1997A&A...322..266A), that for dMe stars the shape of the NaI D emission cores is a much more sensitive indicator of chromospheric thickness (or, equivalently, chromospheric steepness) than is Hα, and, therefore, provides a powerful diagnostic complement to Hα. Finally, we investigate the dependence of the predicted line profiles on the values of the stellar parameters and conclude that the inferred chromospheric pressure is sensitive to the choice of Teff and logg, especially among dMe stars. Specifically, among dMe stars, a model in which the value of Teff is too small or too large by approximately 200K, or in which the value of logg is too large or too small by 0.5dex, will give rise to closest fit values of the column mass density at the location of the Transition Region and Tmin that are too small or too large, respectively, by approximately 0.3dex. As a result, discrepancies between the stellar parameters of our photospheric model and those of the program objects allow us to extract only upper or lower limits for the values of the column mass density at critical points in the chromospheric structure

Abstract Copyright:

Journal keyword(s): stars: late-type - stars: activity - stars: chromospheres - line: formation

Simbad objects: 5

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Number of rows : 5
N Identifier Otype ICRS (J2000)
ICRS (J2000)
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
1 HD 233153 PM* 05 41 30.7306794471 +53 29 23.290604578   11.31   9.343   M1.0V 172 0
2 V* AN Sex RS* 10 12 17.6682499584 -03 44 44.392042932 11.941 10.757 9.264 8.258 7.066 M2V 211 0
3 BD+20 2465 Er* 10 19 36.2808181226 +19 52 12.010446571   10.82 9.52 9.19   dM3 1225 0
4 BD+13 2618 Er* 13 00 46.5566863405 +12 22 32.677229903 12.314 11.233 9.750 8.785 7.653 M0V 324 1
5 BD+00 5017 ** 23 35 00.2767437606 +01 36 19.434711493 12.082 10.893 9.546 8.703 7.879 K7V 144 0

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