A Planet Orbiting the Star ρ Coronae Borealis

@article{Noyes1997APO,
  title={A Planet Orbiting the Star $\rho$ Coronae Borealis},
  author={Robert W. Noyes and Somesh Jha and Sylvain Gereon Korzennik and Mark B Krockenberger and Peter Nisenson and Timothy M. Brown and Edward J. Kennelly and Scott Donald Horner},
  journal={The Astrophysical Journal},
  year={1997},
  volume={483}
}
We report the discovery of near-sinusoidal radial velocity variations of the G0V star ρ CrB, with period 39.6 days and amplitude 67 m s-1. These variations are consistent with the existence of an orbital companion in a circular orbit. Adopting a mass of 1.0 M☉ for the primary, the companion has minimum mass about 1.1 Jupiter masses and orbital radius about 0.23 AU. Such an orbital radius is too large for tidal circularization of an initially eccentric orbit during the lifetime of the star, and… Expand
The Planet Orbiting ρ Coronae Borealis
Continuing precise radial velocity observations of ρ Coronae Borealis have allowed the determination of updated parameters of the 40-day orbit of its Jupiter-mass companion. This confirms theExpand
A Planet with a 3.1 Day Period around a Solar Twin
Doppler measurements from the Keck/HIRES spectrometer of the G3 V star HD 187123 reveal Keplerian variations with a period of 3.097 days and a semiamplitude of 72 m s–1. An orbital fit yields aExpand
Two New Candidate Planets in Eccentric Orbits
Doppler measurements of two G-type main-sequence stars, HD 210277 and HD 168443, reveal Keplerian variations that imply the presence of companions with masses (M sin i) of 1.28 and 5.04 MJ (where MJExpand
The ELODIE survey for northern extra-solar planets - II. A Jovian planet on a long-period orbit around GJ 777 A
We present radial-velocity measurements obtained with the ELODIE and AFOE spectrographs for GJ 777 A (HD 190360), a metal-rich ((Fe/H)= 0.25) nearby (d= 15.9 pc) star in a stellar binary system. AExpand
Extrasolar Planets around Main Sequence Stars
The mass distribution of substellar companions exhibits a steep rise for masses below 5 MJ. Thus, the 14 companions having Msin i = 0.5 { 5 MJ are considered the best candidate planets around mainExpand
DETECTION OF EXTRASOLAR GIANT PLANETS
▪ Abstract Eight extrasolar planet candidates have now been identified, all revealed by Keplerian Doppler shifts in their host stars. The masses (m sin i) lie between 0.5 and 7 MJUP, and theExpand
The Mass Distribution of Extrasolar Planet Candidates and Spectroscopic Binary Low-Mass Companions
Spectroscopic orbits have been reported for nine unseen companions orbiting solar-type stars with minimum possible masses in the range 0.5-10 Jupiter masses. We compare the mass distribution of theseExpand
Analysis of the Hipparcos Measurements of HD 10697: A Mass Determination of a Brown Dwarf Secondary.
  • Zucker, Mazeh
  • Physics, Medicine
  • The Astrophysical journal
  • 2000
TLDR
It is suggested that the secondary of HD 10697 is probably a brown dwarf, orbiting around its parent star at a distance of 2 AU, implying a mass of 38+/-13 MJ for the unseen companion. Expand
Doppler Detection of Extrasolar Planets
We have measured the radial velocities of 540 G and K main sequence stars with a precision of 3−10 ms −1 using the Lick and Keck echelle spectrometers. We had detected 6 companions that have m sin iExpand
Structure and Evolution of Nearby Stars with Planets. I. Short-Period Systems
Using the Yale stellar evolution code, we have calculated theoretical models for nearby stars with planetary-mass companions in short-period nearly circular orbits: 51 Pegasi, τ Bootis, υ Andromedae,Expand
...
1
2
3
4
5
...

References

SHOWING 1-10 OF 29 REFERENCES
Tidal decay of close planetary orbits
The 4.2-day orbit of the newly discovered planet around 51~Pegasi is formally unstable to tidal dissipation. However, the orbital decay time in this system is longer than the main-sequence lifetimeExpand
A Planet Orbiting 47 Ursae Majoris
The G0 V star 47 UMa exhibits very low amplitude radial velocity variations having a period of 2.98 yr, a velocity amplitude of K = 45.5 m s-1, and small eccentricity. The residuals scatter by 11 mExpand
A Jupiter-mass companion to a solar-type star
The presence of a Jupiter-mass companion to the star 51 Pegasi is inferred from observations of periodic variations in the star's radial velocity. The companion lies only about eight millionExpand
The Planet around 51 Pegasi
Doppler measurements of 51 Pegasi have been made from 1995 October through 1996 August, with a precision of 5 m s-1. We find a period of 4.231 days, a velocity amplitude of 56 ± 1 m s-1, and aExpand
Proximity of Jupiter-Like Planets to Low-Mass Stars
  • A. Boss
  • Physics, Medicine
  • Science
  • 1995
TLDR
The sensitivities of astrometric and radial velocity searches for extrasolar planets are strongly dependent on planetary masses and orbits, and radiative hydrodynamic models of protoplanetary disks around low-mass stars show that Jupiter-like planets should form at distances that are only weakly dependent on the stellar mass. Expand
Absence of a planetary signature in the spectra of the star 51 Pegasi
51 Pegasi, one of many nearby Sun-like stars, was undistinguished until the recent detections of apparent variations in its radial velocity, which have been attributed to reflex motion caused by aExpand
Radial velocity observations of the sun at night
We have measured the Doppler shift of the solar spectrum for 5 yr to help demonstrate our ability to detect planets orbiting other stars. The sunlit surface of the Moon provides nighttime access toExpand
Rotation, convection, and magnetic activity in lower main-sequence stars
Rotation periods are reported for 14 main-sequence stars, bringing the total number of such stars with well-determined rotation periods to 41. It is found that the mean level of their Ca n H and KExpand
On the fragmentation of cosmic gas clouds. II - Opacity-limited star formation
Opacity-limited fragmentation of gravitationally collapsing gas clouds is reexamined with inclusion of realistic dust grain opacities and cooling rates. A minimum fragment size of approximately 0.01Expand
Magnetic Field and Rotation in Lower Main-Sequence Stars: An Empirical Time-Dependent Magnetic Bode's Relation?
We find a significant correlation between the magnetic and rotational moments for a sample of 112 lower main-sequence stars. The rotational moment is calculated from measurements of the rotationExpand
...
1
2
3
...