scholarly journals The Keck Planet Search: Detectability and the Minimum Mass and Orbital Period Distribution of Extrasolar Planets

2008 ◽  
Vol 120 (867) ◽  
pp. 531-554 ◽  
Author(s):  
Andrew Cumming ◽  
R. Paul Butler ◽  
Geoffrey W. Marcy ◽  
Steven S. Vogt ◽  
Jason T. Wright ◽  
...  
Keyword(s):  
Orbital Period ◽  
Extrasolar Planets ◽  
Minimum Mass ◽  
Period Distribution

scholarly journals Comparison between Extrasolar Planets and Low-Mass Secondaries

2001 ◽  
Vol 200 ◽  
pp. 519-528 ◽  
Author(s):  
Tsevi Mazeh ◽  
Shay Zucker
Keyword(s):  
Negative Correlation ◽  
Orbital Period ◽  
Extrasolar Planets ◽  
Spectroscopic Binaries ◽  
Statistical Features ◽  
Mass Distributions ◽  
Period Distribution ◽  
Short Period ◽  
Low Mass ◽  
Two Populations

This paper compares the statistical features of the sample of discovered extrasolar planets with those of the secondaries in nearby spectroscopic binaries, in order to enable us to distinguish between the two populations. Based on 32 planet candidates discovered until March 2000, we find that their eccentricity and period distribution are surprisingly similar to those of the binary population, while their mass distribution is remarkably different. The mass distributions definitely support the idea of two distinct populations, suggesting the planet candidates are indeed extrasolar planets. The transition between the two populations probably occurs at 10–30 Jupiter masses. We point out a possible negative correlation between the orbital period of the planets and the metallicity of their parent stars, which holds only for periods less than about 100 days. These short-period systems are characterized by circular or almost circular orbits.

Longevity of moons around habitable planets

2014 ◽  
Vol 13 (4) ◽  
pp. 324-336 ◽  
Author(s):  
Takashi Sasaki ◽  
Jason W. Barnes
Keyword(s):  
Orbital Period ◽  
Extrasolar Planets ◽  
The Sun ◽  
Habitable Zone ◽  
Evolution Theory ◽  
Earth System ◽  
The Moon ◽  
Tidal Dissipation ◽  
Habitable Planets ◽  
Rocky Planets

AbstractWe consider tidal decay lifetimes for moons orbiting habitable extrasolar planets using the constant Q approach for tidal evolution theory. Large moons stabilize planetary obliquity in some cases, and it has been suggested that large moons are necessary for the evolution of complex life. We find that the Moon in the Sun–Earth system must have had an initial orbital period of not slower than 20 h rev−1 for the moon's lifetime to exceed a 5 Gyr lifetime. We assume that 5 Gyr is long enough for life on planets to evolve complex life. We show that moons of habitable planets cannot survive for more than 5 Gyr if the stellar mass is less than 0.55 and 0.42 M⊙ for Qp=10 and 100, respectively, where Qp is the planetary tidal dissipation quality factor. Kepler-62e and f are of particular interest because they are two actually known rocky planets in the habitable zone. Kepler-62e would need to be made of iron and have Qp=100 for its hypothetical moon to live for longer than 5 Gyr. A hypothetical moon of Kepler-62f, by contrast, may have a lifetime greater than 5 Gyr under several scenarios, and particularly for Qp=100.

Angular Momentum Losses and the Orbital Period Distribution of Cataclysmic Variables below the Period Gap: Effects of Circumbinary Disks

2005 ◽  
Vol 635 (2) ◽  
pp. 1263-1280 ◽  
Author(s):  
Bart Willems ◽  
Ulrich Kolb ◽  
Eric L. Sandquist ◽  
Ronald E. Taam ◽  
Guillaume Dubus
Keyword(s):  
Angular Momentum ◽  
Orbital Period ◽  
Cataclysmic Variables ◽  
Period Distribution ◽  
Gap Effects

On the Properties of Galactic Novae and Their Orbital Period Distribution

2004 ◽  
Vol 602 (2) ◽  
pp. 938-947 ◽  
Author(s):  
Lorne A. Nelson ◽  
Keith A. MacCannell ◽  
Ernest Dubeau
Keyword(s):  
Orbital Period ◽  
Period Distribution

The orbital period distribution of subdwarf-B binaries

2004 ◽  
Vol 291 (3) ◽  
pp. 299-306 ◽  
Author(s):  
Luisa Morales-Rueda ◽  
Pierre F.L. Maxted ◽  
Tom R. Marsh
Keyword(s):  
Orbital Period ◽  
Period Distribution

scholarly journals Speckle Observations of TESS Exoplanet Host Stars: Understanding the Binary Exoplanet Host Star Orbital Period Distribution

2021 ◽  
Vol 161 (4) ◽  
pp. 164
Author(s):  
Steve B. Howell ◽  
Rachel A. Matson ◽  
David R. Ciardi ◽  
Mark E. Everett ◽  
John H. Livingston ◽  
...  
Keyword(s):  
Orbital Period ◽  
Period Distribution ◽  
Host Stars

scholarly journals The Orbital Period Distribution of Cataclysmic Variables Found by the SDSS

2011 ◽  
Vol 7 (S282) ◽  
pp. 123-124 ◽  
Author(s):  
John Southworth ◽  
Boris T. Gänsicke ◽  
Elmé Breedt
Keyword(s):  
Angular Momentum ◽  
Orbital Period ◽  
Cataclysmic Variables ◽  
Sloan Digital Sky Survey ◽  
Cataclysmic Variable ◽  
Minimum Period ◽  
Period Distribution ◽  
Sky Survey ◽  
Short Period ◽  
Angular Momentum Loss

AbstractThe orbital period is one of the most accessible observables of a cataclysmic variable. It has been a concern for many years that the orbital period distribution of the known systems does not match that predicted by evolutionary theory. The sample of objects discovered by the Sloan Digital Sky Survey has changed this: it shows the long-expected predominance of short-period objects termed the ‘period spike’. The minimum period remains in conflict with theory, suggesting that the angular momentum loss mechanisms are stronger than predicted.

scholarly journals Discovery of a hot, transiting, Earth-sized planet and a second temperate, non-transiting planet around the M4 dwarf GJ 3473 (TOI-488)

2020 ◽  
Vol 642 ◽  
pp. A236
Author(s):  
J. Kemmer ◽  
S. Stock ◽  
D. Kossakowski ◽  
A. Kaminski ◽  
K. Molaverdikhani ◽  
...  
Keyword(s):  
Orbital Period ◽  
Emission Spectroscopy ◽  
Thermal Emission ◽  
Mass Measurement ◽  
Minimum Mass ◽  
Dwarf Star ◽  
Dynamical Mass ◽  
Planetary Mass ◽  
Thermal Emission Spectroscopy

We present the confirmation and characterisation of GJ 3473 b (G 50–16, TOI-488.01), a hot Earth-sized planet orbiting an M4 dwarf star, whose transiting signal (P = 1.1980035 ± 0.0000018 d) was first detected by the Transiting Exoplanet Survey Satellite (TESS). Through a joint modelling of follow-up radial velocity observations with CARMENES, IRD, and HARPS together with extensive ground-based photometric follow-up observations with LCOGT, MuSCAT, and MuSCAT2, we determined a precise planetary mass, Mb = 1.86 ± 0.30 M⊕, and radius, Rb = 1.264 ± 0.050 R⊕. Additionally, we report the discovery of a second, temperate, non-transiting planet in the system, GJ 3473 c, which has a minimum mass, Mc sin i = 7.41 ± 0.91 M⊕, and orbital period, Pc = 15.509 ± 0.033 d. The inner planet of the system, GJ 3473 b, is one of the hottest transiting Earth-sized planets known thus far, accompanied by a dynamical mass measurement, which makes it a particularly attractive target for thermal emission spectroscopy.

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