NEXXUS: A comprehensive ROSAT survey of coronal X-ray emission among nearby solar-like stars

By J. Schmitt, C. Liefke. 2003

185 citations recorded by the source corpus.

We present a final summary of all ROSAT X-ray observations of nearby stars. All available ROSAT observations with the ROSAT PSPC, HRI and WFC have been matched with the CNS4 catalog of nearby stars and the results gathered in the Nearby X-ray and XUV-emitting Stars data base, available via www from the Home Page of the Hamburger Sternwarte at the URL http://www.hs.uni-hamburg.de/DE/For/Gal/Xgroup/nexxus. New volume-limited samples of F/G-stars (dlim = 14 pc), K-stars (dlim = 12 pc), and M-stars (dlim = 6 pc) are constructed within which detection rates of more than 90% are obtained; only one star (GJ 1002) remains undetected in a pointed follow-up observation. F/G-stars, K-stars and M-stars have indistinguishable surface X-ray flux distributions, and the lower envelope of the observed distribution at FX ≈ 10 4 erg/cm 2 /s is the X-ray flux level observed in solar coronal holes. Large amplitude variations in X-ray flux are uncommon for solar-like stars, but maybe more common for stars near the bottom of the main sequence; a large amplitude flare is reported for the M star LHS 288. Long term X-ray light curves are presented for α Cen A/B and Gl 86, showing variations on time scales of weeks and demonstrating that α Cen B is a flare star.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/859a76ea0c46efa45db1602020221d9b987ff747

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Citations in the corpus

• The habitability of Proxima Centauri b. I. Irradiation, rotation and volatile inventory from formation to the present (2016, methodology): “X-ray emission of Proxima was observed with ROSAT and XMM. Hünsch et al. (1999) report log LX = 27.2 erg s−1 from a ROSAT observation, and Schmitt & Liefke (2004) report log LX = 26.9 erg s−1 for ROSAT PSPC and log LX = 27.4 erg s−1 for an XMM observation.”
• The First Direct Measurements of Surface Magnetic Fields on Very Low Mass Stars (2006, unknown): “0 2390 12 4.6 29.05 −4.00 −3.50d > 3.9 aDelfosse et al. (1998) bFleming et al. (1995) cLX from Schmitt & Liefke (2004), Lbol from the calibration of Delfosse et al. (1998) with MV and R− I from Gliese & Jahreiss (1991) dFleming et al. (1993) eFleming et al. (2003)”
• Large-scale magnetic topologies of late M dwarfs★: Magnetic topologies of late M dwarfs (2010, methodology): “All these stars are known to show signs of activity in Hα or X-rays (e.g. Gizis et al. 2002; Schmitt & Liefke 2004), and photospheric magnetic fields have been measured on most of them from the analysis of Zeeman broadening in molecular bands (see below).”
• EVIDENCE FOR MAGNETIC FLUX SATURATION IN RAPIDLY ROTATING M STARS (2008, methodology): “This value is calculated from the X-ray luminosity taken from Schmitt & Liefke (2004).”
• The Evolution of X-Ray Emission in Young Stars (2005, methodology): “For older Galactic disk stars, we use the NEXXUS database (Schmitt & Liefke 2004) provides updated ROSAT X-ray and optical data (including accurate HIPPARCOS parallaxes) for a well-defined volume-limited samples of nearby field stars.”
• THE STELLAR-ACTIVITY–ROTATION RELATIONSHIP AND THE EVOLUTION OF STELLAR DYNAMOS (2011, background): “This high-temperature rarefied thermal plasma, first observed on the Sun, has been detected from nearly all classes of low-mass stars at levels of LX/Lbol ∼ 10−8 − 10−3 (Schmitt & Liefke 2004).”
• The Origin of T Tauri X-Ray Emission: New Insights from the Chandra Orion Ultradeep Project (2005, methodology): “Awell-suited comparison sample is the NEXXUS database (Schmitt & Liefke 2004), which provides updated ROSAT X-ray and optical data (including accurate Hipparcos parallaxes) for nearby field stars.”
• Stellar Lyα Emission Lines in the Hubble Space Telescope Archive: Intrinsic Line Fluxes and Absorption from the Heliosphere and Astrospheres (2005, methodology): “Over half the X-ray fluxes are taken from the nearby star survey of Schmitt & Liefke (2004).”
• The Activity and Variability of the Sun and Sun-like Stars. I. Synoptic Ca II H and K Observations (2007, background): “Although this star exhibits one of the best-defined cycles of the MWO stars (9:6 0:1 yr; B95), its X-ray luminosity is quite low relative to stars of its type, at only 0.34 dex above HD 10700 in the RASS observations (Schmitt & Liefke 2004).”
• Evaporation of the planet HD 189733b observed in H I Lyman-α (2010, background): “However, for a K-type star, it can be estimated to be in the range 1 to 100 times the solar EUV flux (e.g., Schmitt & Liefke 2004).”
• The stellar rotation–activity relationship in fully convective M dwarfs (2018, methodology): “2.5 ROSAT observations of additional sources Two objects, GJ 699 and GJ 551, were observed by ROSAT, with X-ray fluxes presented by Schmitt & Liefke (2004).”