ausblenden:
Schlagwörter:
stars: activity; stars: low-mass; stars: late-type; stars:
chromospheres; Astrophysics - Solar and Stellar Astrophysics;
Astrophysics - Earth and Planetary Astrophysics
Zusammenfassung:
Context. With the recent surge of planetary surveys focusing on detecting Earth-mass planets around M dwarfs, it is becoming more important to understand chromospheric activity in M dwarfs. Stellar chromospheric calcium emission is typically measured using the R'HK calibrations of Noyes et al. (1984), which are only valid for 0.44 ≤ B - V ≤ 0.82. Measurements of calcium emission for cooler dwarfs B - V ≥ 0.82 are difficult because of their intrinsic dimness in the blue end of the visible spectrum.
Aims: We measure the absolute Ca II H & K and Hα flux of a sample of 110 HARPS M dwarfs and also extend the calibration of R'HK to the M dwarf regime using PHOENIX stellar atmosphere models.
Methods: We normalized a template spectrum with a high signal-to-noise ratio that was obtained by coadding multiple spectra of the same star to a PHOENIX stellar atmosphere model to measure the chromospheric Ca II H & K and Ha flux in physical units. We used three different Teff calibrations and investigated their effect on Ca II H & K and Hα activity measurements. We performed conversions of the Mount Wilson S index to R'HK as a function of effective temperature for the range 2300 K ≤ Teff ≤ 7200 K. Last, we calculated continuum luminosity χ values for Ca II H & K and Hα in the same manner as West & Hawley (2008) for -1.0 ≤ [Fe/H] ≤ + 1.0 in steps of Δ [Fe/H] = 0.5.
Results: We compare different Teff calibrations and find ΔΤeff ~ several 100 K for mid- to late-M dwarfs. Using these different Teff calibrations, we establish a catalog of log R'HK and ''Hα/ℱbol measurements for 110 HARPS M dwarfs. The difference between our results and the calibrations of Noyes et al. (1984) is Δ log R'HK = 0.01 dex for a Sun-like star. Our χ values agree well with those of West & Hawley (2008). We confirm that the lower boundary of chromospheric Ca II H and K activity does not increase toward later-M dwarfs: it either stays constant or decreases, depending on the Teff calibration used. We also confirm that for Ha, the lower boundary of chromospheric flux is in absorption for earlier -M dwarfs and fills into the continuum toward later M dwarfs.
Conclusions: We confirm that we can effectively measure R'HK in M dwarfs using template spectra with a high signal-to-noise ratio. We also conclude that our calibrations are a reliable extension of previous R'HK calibrations, and effective temperature calibration is the main source of error in our activity measurements.
