Planetary Companions to HD 12661, HD 92788, and HD 38529 and Variations in Keplerian Residuals of Extrasolar Planets

By Debra A. Fischer, G. Marcy, R. P. Butler, S. Vogt, S. Frink, K. Apps. 2001

133 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/37e5cdcb0a5ebf118385321830d5ea42c2c6cb06

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Citations in the corpus

Two New Planets from the Anglo-Australian Planet Search (2001, background): “In addition, Fischer et al. (2001) have shown several class IV subgiants are stable at the 6 m s~1 level.”
A Pair of Resonant Planets Orbiting GJ 876 (2001, background): “It appears that stars with planets have a high occurrence rate, at least 50%, of harboring more distant substellar companions, planetary or otherwise (Fischer et al. 2001 ; Marcy et al. 2001b).”
SECULAR CHAOS AND THE PRODUCTION OF HOT JUPITERS (2010, background): “They should be roaming at large distances (outside a few AU) and remain to be detected—some may have already shown up as RV residuals in hot Jupiter systems (Fischer et al. 2001; Wright et al. 2009).”
On the Radii of Extrasolar Giant Planets (2003, background): “Fischer et al. (2001) have noted that the inclusion of a second planet into a RV fit generally causes the fitted eccentricity of the first planet to decline.”
Circumstellar Dust Disks in Taurus-Auriga: The Submillimeter Perspective (2005, background): “Radial velocity surveys suggest that roughly 10% of stars harbor a gas giant planet within a few AU (e.g., Marcy et al. 2005), with the prospect that better sensitivity to long-period planets could significantly increase that fraction (e.g., Fischer et al. 2001).”
Secular Evolution of Hierarchical Planetary Systems (2002, background): “There are also indications that about half of the stars with one known planet are likely to have additional detectable distant companions (Fischer et al. 2001).”
Planet formation and migration (2005, background): “Among the candidate systems with large radial velocity drifts potentially due to a companion selected by Fischer et al (2001) was HD 38529, which has a planet with mp sin i = 0.76 MJ, a = 0.13 AU and e = 0.27.”
The Keck Planet Search: Detectability and the Minimum Mass and Orbital Period Distribution of Extrasolar Planets (2008, background): “Over 25 multiple planet systems are known, with many other single planet systems showing a long term velocity trend likely indicating a second planet with long orbital period (Fischer et al. 2001).”
TEN NEW AND UPDATED MULTIPLANET SYSTEMS AND A SURVEY OF EXOPLANETARY SYSTEMS (2008, background): “Fischer et al. (1999) reported a 7.1 d, M sin i = 1.4MJup planet orbiting HD 217107, and Fischer et al. (2001) described a linear trend superimposed on the Lick and Keck radial velocities.”
Structure and Evolution of Nearby Stars with Planets. II. Physical Properties of ~1000 Cool Stars from the SPOCS Catalog (2006, background): “The inner planet HD38529b (Mpl = 0.78MJ, P = 14.3 days) was discovered by Fischer et al. (2001).”
Five New Multicomponent Planetary Systems (2005, methodology): “We have also continued to obtain velocities for HD 217107 from Lick Observatory, contiguous with the velocity set described by Fischer et al. (2001).”
The CORALIE survey for southern extra-solar planets. XII. Orbital solutions for 16 extra-solar planets discovered with CORALIE (2003, methodology): “Simultaneous independent discoveries have been made for 3 of our candidates: by Fischer et al. (2001) for HD 92788 and by Jones et al. (2002) for HD 196050 and 3 The CORALIE numerical mask used in the cross correlation for the velocity estimate was built from a K0-dwarf spectrum.”
Quantifying the Uncertainty in the Orbits of Extrasolar Planets (2003, background): “Several stars presently known to harbor one planet are expected to reveal additional planets in longer period orbits (Fischer et al. 2001).”
DHP Framework: Digital Health Passports Using Blockchain - Use case on international tourism during the COVID-19 pandemic (2004, background): “About 10 per cent of the stars with known planetary companions have more than one planet, while possibly as much as 50 per cent of them show a trend in radial velocity indicative of additional planets (Fischer et al. 2001).”
FRIENDS OF HOT JUPITERS. I. A RADIAL VELOCITY SEARCH FOR MASSIVE, LONG-PERIOD COMPANIONS TO CLOSE-IN GAS GIANT PLANETS (2013, background): “The sample of radial velocity planets provides a better basis for comparison, as it includes many systems with long-term radial velocity monitoring capable of detecting massive companions on long-period orbits (e.g., Fischer et al. 2001; Wright et al. 2007, 2009).”
THE TWENTY-FIVE YEAR LICK PLANET SEARCH (2013, unknown): “…50554 b, HD 105252 b (Fischer et al. 2002), one of the first cold, sub-Saturn mass planets, HD 3651 b (Fischer et al. 2003), HD 49079 b, HD 12661 b, c, HD 38529 b, c (Fischer et al. 2001, 2003), and HD 30562 b, HD 86264b, HD 87883 b, HD 89307 b, HD 148427 b, and HD 196885A b (Fischer et al. 2009).”