The M Dwarf GJ 436 and its Neptune‐Mass Planet

The M Dwarf GJ 436 and its Neptune - Mass Planet

We determine stellar parameters for the M dwarf GJ 436 that hosts a Neptunemass planet. We employ primarily spectral modeling at low and high resolution, examining the agreement between model and observed optical spectra of five comparison stars of type, M0-M3. Modeling high resolution optical spectra suffers from uncertainties in TiO transitions, affecting the predicted strengths of both atomi...

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0 v 2 4 D ec 2 00 6 The M Dwarf GJ 436 and its Neptune - Mass Planet

We determine stellar parameters for the M dwarf GJ 436 that hosts a Neptunemass planet. We employ primarily spectral modeling at low and high resolution, examining the agreement between model and observed optical spectra of five comparison stars of type, M0-M3. Modeling high resolution optical spectra suffers from uncertainties in TiO transitions, affecting the predicted strengths of both atomi...

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Up to four planets around the M dwarf GJ 163

Context. Exoplanet Doppler surveys are currently the most efficient means to detect low-mass companions to nearby stars. Among these stars, the light M dwarfs provide the highest sensitivity to detect low-mass exoplanet candidates. Evidence is accumulating that a substantial fraction of these low-mass planets are found in high-multiplicity planetary systems. GJ 163 is a nearby inactive M dwarf ...

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ar X iv : a st ro - p h / 06 08 26 0 v 1 1 1 A ug 2 00 6 The M Dwarf GJ 436 and its Neptune - Mass Planet

We determine stellar parameters for the M dwarf GJ 436 that hosts a Neptunemass planet. We employ primarily spectral modeling at low and high resolution, examining the agreement between model and observed optical spectra of five comparison stars of type, M0-M3. Modeling high resolution optical spectra suffers from uncertainties in TiO transitions, affecting the predicted strengths of both atomi...

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GJ 2069 A , a new M dwarf eclipsing binary ?

We have discovered a third detached M dwarf eclipsing binary system, for which we present an accurate radial velocity orbit and a preliminary light curve. From those data, we derive individual masses (0.433 and 0.397 M ) with 0.4% accuracy, the most accurate to date for M dwarfs. Both stars are clearly sub-luminous for their mass, compared with solar metallicity stellar models or empirical mass...

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The M Dwarf GJ 436 and its Neptune‐Mass Planet

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