A Chandra/LETGS Survey of Main Sequence Stars

Abstract

We analyze the X-ray spectra of 19 main sequence stars observed by Chandra using its LETGS configuration. Emission measure (EM) distributions are computed based on emission line measurements, an analysis that also yields evaluations of coronal abundances. The use of newer atomic physics data results in significant changes compared to past published analyses. The stellar EM distributions correlate with surface X-ray flux (F_X) in a predictable way, regardless of spectral type. Thus, we provide EM distributions as a function of F_X, which can be used to estimate the EM distribution of any main sequence star with a measured broadband X-ray luminosity. Comparisons are made with solar EM distributions, both full-disk distributions and spatially resolved ones from active regions (ARs), flares, and the quiet Sun. For moderately active stars, the slopes and magnitudes of the EM distributions are in excellent agreement with those of solar ARs for log T<6.6, suggesting that such stars have surfaces completely filled with solar-like ARs. A stellar surface covered with solar X-class flares yields a reasonable approximation for the EM distributions of the most active stars. Unlike the EM distributions, coronal abundances are very spectral-type dependent, and we provide relations with surface temperature for both relative and absolute abundances. Finally, the coronal abundances of the exoplanet host star Tau Boo A (F7 V) are anomalous, and we propose that this is due to the presence of the exoplanet.

arXiv comment30 pages, 12 figures, to appear in The Astrophysical Journal

References in corpus (82)

• The chemical composition of the Sun
• Intrinsic Colors, Temperatures, and Bolometric Corrections of Pre-Main Sequence Stars
• The NextGen Model Atmosphere grid for $3000\le \Teff \le 10000\K$
• Ionization balance for optically thin plasmas: rate coefficients for all atoms and ions of the elements H to Ni
• How to Constrain Your M Dwarf: measuring effective temperature, bolometric luminosity, mass, and radius
• Stellar Diameters and Temperatures II. Main Sequence K & M Stars
• The Geneva-Copenhagen Survey of the Solar neighbourhood III. Improved distances, ages, and kinematics
• Large-scale magnetic topologies of mid-M dwarfs
• The signature of orbital motion from the dayside of the planet tau Bootis b
• X-ray astronomy of stellar coronae (Review)
• The Structure of the Local Interstellar Medium V: Electron Densities
• S4N: A Spectroscopic Survey of Stars in the Solar Neighborhood
• The FIP and Inverse FIP Effects in Solar and Stellar Coronae
• Gaia FGK Benchmark Stars: Effective temperatures and surface gravities
• Stellar Lyman-alpha Emission Lines in the Hubble Space Telescope Archive: Intrinsic Line Fluxes and Absorption from the Heliosphere and Astrospheres
• The On/Off Nature of Star-Planet Interactions
• X-Ray Spectroscopy of Stars
• Hot Jupiters and Hot Spots: The Short- and Long-term Chromospheric Activity on Stars with Giant Planets
• Resolving the Xi Boo Binary with Chandra, and Revealing the Spectral Type Dependence of the Coronal "FIP Effect"
• NEXXUS: A comprehensive ROSAT survey of coronal X-ray emission among nearby solar-like stars
• A Unified Picture of the FIP and Inverse FIP Effects
• Stellar Diameters and Temperatures I. Main Sequence A, F, & G Stars
• The "Solar Model Problem" Solved by the Abundance of Neon in Stars of the Local Cosmos
• Magnetic cycles of the planet-hosting star tauBootis
• Coronal Evolution of the Sun in Time: High-Resolution X-Ray Spectroscopy of Solar Analogs with Different Ages
• A Systematic Survey of High Temperature Emission in Solar Active Regions
• Gaia FGK benchmark stars: abundances of alpha and iron-peak elements
• The diameters of Alpha Centauri A and B - A comparison of the asteroseismic and VINCI/VLTI views
• Flares from small to large: X-ray spectroscopy of Proxima Centauri with XMM-Newton
• Extrasolar Giant Planets and X-ray Activity
• Non-WKB Models of the FIP Effect: Implications for Solar Coronal Heating and the Coronal Helium and Neon Abundances
• High-resolution X-ray spectroscopy of Procyon by Chandra and XMM-Newton
• The Density of Coronal Plasma in Active Stellar Coronae
• Indications for an influence of Hot Jupiters on the rotation and activity of their host stars
• A Study of the Coronal Plasma in RS CVn binary systems
• X-Ray Spectroscopy of II Pegasi: Coronal Temperature Structure, Abundances, and Variability
• The magnetic field of the planet-hosting star $\tau$ Bootis
• MOST detects variability on tau Bootis possibly induced by its planetary companion
• Magnetic cycles at different ages of stars
• X-ray properties of active M dwarfs as observed by XMM-Newton
• Possible constraints on exoplanet magnetic field strengths from planet-star interaction
• The corona of HD 189733 and its X-ray activity
• The Ne/O abundance ratio in the quiet Sun
• Non-WKB Models of the FIP Effect: The Role of Slow Mode Waves
• Neon Lights Up a Controversy: the Solar Ne/O Abundance
• Resolving the Effects of Rotation in Altair with Long-Baseline Interferometry
• Measurements of Absolute Abundances in Solar Flares
• The Evolving Magnetic Topology of $\tau$ Boötis
• On the detectability of star-planet interaction
• A coordinated optical and X-ray spectroscopic campaign on HD179949: searching for planet-induced chromospheric and coronal activity
• Interactions of the magnetospheres of stars and close-in giant planets
• A correlation between host star activity and planet mass for close-in extrasolar planets?
• Element abundance ratios in the quiet Sun transition region
• Parent Stars of Extrasolar Planets. VIII. Chemical Abundances for 18 Elements in 31 Stars
• From Radio to X-ray: The Quiescent Atmosphere of the dMe Flare Star EV Lacertae
• An Improved Age-Activity Relationship for Cool Stars older than a Gigayear
• No X-rays from WASP-18. Implications for its age, activity, and the influence of its massive hot Jupiter
• The Structure of the Local Interstellar Medium. VI. New MgII, FeII, and MnII Observations Toward Stars Within 100 Parsecs
• Testing EUV/X-ray Atomic Data for the Solar Dynamics Observatory
• Fe XVII X-ray Line Ratios for Accurate Astrophysical Plasma Diagnostics
• Altair - the 'hottest' magnetically active star in X-rays
• A Solar cycle correlation of coronal element abundances in Sun-as-a-star observations
• The Absolute Abundance of Iron in the Solar Corona
• A search for star-planet interactions in the upsilon Andromedae system at X-ray and optical wavelengths
• Coronal Sources of the Solar F${}_{10.7}$ Radio Flux
• Stellar Winds and Coronae of Low-mass Pop. II/III Stars
• On the chromospheric activity of stars with planets
• The Ups and Downs of Alpha Centauri
• The Coronal Abundance Anomalies of M Dwarfs
• Coronal Emission Measures and Abundances for Moderately Active K Dwarfs Observed by Chandra
• Asymmetric Surface Brightness Distribution of Altair Observed with the Navy Prototype Optical Interferometer
• Coronal properties of the EQ Peg binary system
• Suppressed Far-UV Stellar Activity and Low Planetary Mass Loss in the WASP-18 System
• Neon and oxygen in low activity stars: towards a coronal unification with the Sun
• X-ray spectroscopy of the unsteady quiescent corona of AD Leo with Chandra
• The Slowly Varying Corona: I --- Daily Differential Emission Measure Distributions Derived from EVE Spectra
• The Coronal Abundances of Mid-F Dwarfs
• Photospheric and coronal abundances in solar-type stars: the peculiar case of Tau Bootis
• The coronal Ne/O abundance of alpha Centauri
• Coronae of Stars with Super Solar Elemental Abundances
• Long-term Variation of the Corona in Quiet Regions
• The magnetic future of the Sun

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• Transient Inverse-FIP Plasma Composition Evolution within a Confined Solar Flare
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• Inverse FIP Effects in Giant Solar Flares Found from Earth X-Ray Albedo with Suzaku/XIS
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