On the Mass-Period Correlation of the Extrasolar Planets

By S. Zucker, T. Mazeh. 2002

147 citations recorded by the source corpus.

We report on a possible correlation between the masses and periods of the extrasolar planets, manifested as a paucity of massive planets with short orbital periods. Monte Carlo simulations show the effect is significant and is not solely due to an observational selection effect. We also show the effect is stronger than the one already implied by published models that assumed independent power-law distributions for the masses and periods of the extrasolar planets. Planets found in binary stellar systems may have an opposite correlation. The difference is highly significant despite the small number of planets in binary systems. We discuss the paucity of short-period massive planets in terms of some theories for the close-in giant planets. Almost all models can account for the deficit of massive planets with short periods, in particular the model that assumes migration driven by a planet-disk interaction, if the planet masses do not scale with their disk masses.

Subfields: Astronomy and Astrophysics, Instrumentation, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/576ba9a4d53bd0b81fa5f7429ddaf851223356c4

How researchers see this paper

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In Astronomy and Astrophysics

1. C. Mordasini
2. Nuno C. Santos
3. M. Mayor
4. S. Udry
5. Y. Alibert
6. M. Perryman
7. Jon Fortney
8. J. Southworth

In Instrumentation

1. J. Southworth
2. Nuno C. Santos
3. S. Udry
4. S. Naoz
5. A. Tokovinin
6. M. Mayor
7. C. Mordasini
8. Sara Seager

In Statistical and Nonlinear Physics

1. S. Naoz
2. Y. Lithwick
3. Yanqin Wu
4. C. Mordasini
5. F. Rasio
6. M. Mayor
7. W. Farr
8. Nuno C. Santos

Citations in the corpus

• Statistical properties of exoplanets. III. Planet properties and stellar multiplicity (2004, background): “Two interesting features emerge from this plot: there are no short-period extrasolar planets with a mass M2 sin i 5 MJ, and the most massive shortperiod planets are almost all found in multiple star systems (Udry et al. 2002; Zucker & Mazeh 2002; Paper I).”
• The Effect of Tidal Inflation Instability on the Mass and Dynamical Evolution of Extrasolar Planets with Ultrashort Periods (2003, background): “Whether the paucity of the massive close-in Jovian planets (Zucker & Mazeh 2002) results from our scenario is left undetermined until more simulations are carried out for the close-in planets with Mp > 1MJ (but, see Paetzold & Rauer 2002 and Jiang et al. 2003for another model).”
• ON THE FORMATION OF HOT JUPITERS IN STELLAR BINARIES (2012, background): “Close-in giant planets tend to be found preferentially in binary stellar systems (Zucker & Mazeh 2002; Udry & Santos 2007).”
• Planet formation and migration (2005, background): “It has further been pointed out that planets more massive than 2 MJ at a 4 AU are actually members of binary star systems (Zucker & Mazeh 2002).”
• Planet Migration and Binary Companions: The Case of HD 80606b (2003, background): “Other Planetary Systems Zucker & Mazeh (2002) showed that planets in binaries are statistically different from those around isolated stars in their period-mass distribution.”
• Extrasolar planet population synthesis - II. Statistical comparison with observations (2009, background): “It also naturally causes an absence of very massive planets at small distances from the star, as observed (Zucker & Mazeh 2002).”
• Spectroscopic [Fe/H] for 98 extra-solar planet-host stars. Exploring the probability of planet formation (2003, background): “1 See e.g. table ath tp://obswww.unige.ch/Exoplanets for a continuously updated version 2001; Zucker & Mazeh 2002; Udry et al. 2003; Santos et al. 2003a; Eggenberger et al. 2003).”
• Properties of planets in binary systems - The role of binary separation (2006, background): “Indeed, Zucker & Mazeh (2002) considered in their statistical analysis only binaries whose projected separation is smaller than 1000 AU, then excluding very wide binaries included in increasingly larger number in later studies.”
• The HARPS survey for southern extra-solar planets. II. A 14 Earth-masses exoplanet around μ Arae (2004, background): “…number of known systems is, however, giving the possibility to explore their properties from a statistical point of view (e.g. Santos et al. 2001; Zucker & Mazeh 2002; Udry et al. 2003; Eggenberger et al. 2004), and the observational and theoretical approaches are now starting to converge (e.g.…”
• Tertiary Companions to Close Spectroscopic Binaries (2006, background): “A distant (stellar) companion enhances planet growth and migration (Zucker & Mazeh 2002; Udry et al. 2003; Eggenberger et al. 2004), possibly in an analogous way to multiple-star formation as envisioned by Larson (2002) and others.”
• The CORALIE survey for southern extra-solar planets. XII. Orbital solutions for 16 extra-solar planets discovered with CORALIE (2003, background): “Also the mass-period relation of exoplanets, checked for statistical significance by Zucker & Mazeh (2002) and further discussed in Udry et al. (2003d), is apparent in 5 Long-period candidates on low-eccentricity orbits (closer to the giant planets in our solar systems) are however more and more…”
• Runaway Migration and the Formation of Hot Jupiters (2003, methodology): “A recent analysis by Zucker & Mazeh (2002) indicates a paucity of planets with masses exceeding a Jupiter mass at small periods of roughly a few days, while sub-Jovian mass planets tend to cluster at these small periods.”
• The missing link: A 4-day period transiting exoplanet around OGLE-TR-111 (2004, background): “It corresponds to the pile-up of periods near 3-4 days observed in Doppler exoplanet surveys (Udry, Mayor & Santos 2003), and its small mass is near the median of Pegasid masses, that are found to be much lighter on average than longer-period gas giants (Zucker & Mazeh 2002).”
• The CORALIE survey for southern extra-solar planets - IX. A 1.3-day period brown dwarf disguised as a planet (2002, background): “Recently, Zucker & Mazeh (2002) discussed an interesting correlation between the planetary mass and the orbital period.”
• A Unique Solution of Planet and Star Parameters from an Extrasolar Planet Transit Light Curve (2002, background): “Selection of the best candidates is especially important if the tendency for planets with small orbital distances to have low mass (Zucker & Mazeh 2002) — and hence low radial velocity amplitudes — is generally true.”
• SECULAR CHAOS AND THE PRODUCTION OF HOT JUPITERS (2010, background): “Hot Jupiters appear to be less massive than more distant planets (Pätzold & Rauer 2002; Zucker & Mazeh 2002).”
• ATMOSPHERIC ESCAPE FROM HOT JUPITERS (2008, background): “In fact, hot Jupiters are observed to have systematically lower masses than extrasolar planets at larger distances from their stars (Zucker & Mazeh 2002).”