Dynamical Interactions Make Hot Jupiters in Open Star Clusters

Shara, Michael M.; Hurley, Jarrod R.; Mardling, Rosemary A.

doi:10.3847/0004-637x/816/2/59

Cited by 84 publications

(57 citation statements)

References 54 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Close stellar fly-by or binary companions can alter the structure of any planetary system and may also trigger subsequent planet-planet scattering over very long timescales (Davies et al 2014;Malmberg et al 2011). This leads to the ejection of some planets, but it also seems to favour the conditions for the formation of HJs (Shara et al 2016). As predicted by such mechanisms, M67 HJs show orbits with non-zero eccentricity, which is also true for the HJ found in the Hyades.…”

Section: Frequency Of Hot Jupiters In Ocsmentioning

confidence: 89%

“…M67 has more than 1400 stars at present, it is dominated by a high fraction of binaries (Davenport & Sandquist 2010) after loosing at least three quarters of its original stellar mass, and has suffered mass segregation. Shara et al (2016) have recently completed N-body simulations for a case similar to the one of M67, but with only a 10% of binaries, finding that HJs can be produced in 0.4% of cluster planetary systems when only considering initial fly-by encounters. This fraction is smaller than what we find in M67, and the influence of other migration mechanisms probably needs to be considered as well to explain our results.…”

Section: Frequency Of Hot Jupiters In Ocsmentioning

confidence: 99%

“…have shown that a planetary system inside a crowded birthenvironment can be strongly destabilized by stellar encounters and dynamical interaction, which also favours the formation of HJs (Davies et al 2014;Malmberg et al 2011;Shara et al 2016). Open clusters (OCs) hold great promise as laboratories in which properties of exoplanets and theories of planet formation and migration can be explored.…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Search for giant planets in M67

Brucalassi

Pasquini

Saglia

et al. 2016

A&A

View full text Add to dashboard Cite

Since 2008 we used high-precision radial velocity (RV) measurements obtained with different telescopes to detect signatures of massive planets around main-sequence and evolved stars of the open cluster (OC) M67. We aimed to perform a long-term study on giant planet formation in open clusters and determine how this formation depends on stellar mass and chemical composition. A new hot Jupiter (HJ) around the main-sequence star YBP401 is reported in this work. An update of the RV measurements for the two HJ host-stars YBP1194 and YBP1514 is also discussed. Our sample of 66 main-sequence and turnoff stars includes 3 HJs, which indicates a high rate of HJs in this cluster (5.6 +5.4 −2.6 % for single stars and 4.5% +4.5 −2.5 % for the full sample). This rate is much higher than what has been discovered in the field, either with RV surveys or by transits. High metallicity is not a cause for the excess of HJs in M67, nor can the excess be attributed to high stellar masses. When combining this rate with the non-zero eccentricity of the orbits, our results are qualitatively consistent with a HJ formation scenario dominated by strong encounters with other stars or binary companions and subsequent planet-planet scattering, as predicted by N-body simulations.

show abstract

Section: Frequency Of Hot Jupiters In Ocsmentioning

confidence: 89%

Section: Frequency Of Hot Jupiters In Ocsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Search for giant planets in M67

Brucalassi

Pasquini

Saglia

et al. 2016

A&A

View full text Add to dashboard Cite

show abstract

“…As a consequence, we should have a large number of systems with a HJ and a second giant planet on an outer eccentric orbit with respect to the second case. Recent simulations have tried to tackle the problem by determining the expected frequency of such systems (Hao et al 2013;Li & Adams 2015) or advocating a cluster origin for several field stars with planetary systems similar to that of Pr 0211 (Shara et al 2016).…”

Section: Discussionmentioning

confidence: 99%

The GAPS programme with HARPS-N at TNG

Malavolta

Nascimbeni

Piotto

et al. 2016

A&A

100

View full text Add to dashboard Cite

Context. Open cluster (OC) stars share the same age and metallicity, and, in general, their age and mass can be estimated with higher precision than for field stars. For this reason, OCs are considered an important laboratory to study the relation between the physical properties of the planets and those of their host stars, and the evolution of planetary systems. However, only a handful of planets have been discovered around OC mainsequence stars so far, all of them in single-planet systems. For this reason we started an observational campaign within the GAPS collaboration to search for and characterize planets in OCs Aims. We monitored the Praesepe member Pr 0211 to improve our knowledge of the eccentricity of the hot Jupiter (HJ) that is already known to orbit this star and search for additional intermediate-mass planets. An eccentric orbit for the HJ would support a planet-planet scattering process rather than a disk-driven migration after its formation. Methods. From 2012 to 2015, we collected 70 radial velocity (RV) measurements with HARPS-N and 36 with TRES of Pr 0211. Simultaneous photometric observations were carried out with the robotic STELLA telescope to characterize the stellar activity. We discovered a long-term trend in the RV residuals that we show as being due to the presence of a second, massive, outer planet. Orbital parameters for the two planets are derived by simultaneously fitting RVs and photometric light curves, with the activity signal modelled as a series of sinusoids at the rotational period of the star and its harmonics. Results. We confirm that Pr 0211b has a nearly circular orbit (e = 0.02 ± 0.01), with an improvement of a factor two with respect to the previous determination of its eccentricity, and estimate that Pr 0211c has a mass M p sin i = 7.9 ± 0.2 M J , a period P > 3500 days and a very eccentric orbit (e > 0.60). This kind of peculiar system may be typical of open clusters if the planet-planet scattering phase, which lead to the formation of HJs, is caused by stellar encounters rather than by unstable primordial orbits. Pr 0211 is the first multi-planet system discovered around an OC star.

show abstract

“…Multiplanet systems are substantially more fragile than singleplanet systems. Small perturbation of an outer planet can induce strong gravitational interactions with other planet(s) in the system, which may result in a reconfiguration of the system, in the ejection of one or more planets, or in a physical star-planet or planet-planet collision (see, e.g., Hao et al 2013;Shara et al 2014). Moreover, we have not included primordial binaries.…”

Section: Conclusion and Discussionmentioning

confidence: 99%

The dynamical fate of planetary systems in young star clusters

Zheng

Kouwenhoven

Wang

2015

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

We carry out N -body simulations to examine the effects of dynamical interactions on planetary systems in young open star clusters. We explore how the planetary populations in these star clusters evolve, and how this evolution depends on the initial amount of substructure, the virial ratio, the cluster mass and density, and the initial semi-major axis of the planetary systems. The fraction of planetary systems that remains intact as a cluster member, f BPS , is generally well-described by the functional formis the fraction of stars that escapes from the cluster, a 0 the critical semi-major axis for survival, and c a measure for the width of the transition region. The effect of the initial amount of substructure over time t can be quantified as f BPS = A(t) + B(D), where A(t) decreases nearly linearly with time, and B(D) decreases when the clusters are initially more substructured. Provided that the orbital separation of planetary systems is smaller than the critical value a 0 , those in clusters with a higher initial stellar density (but identical mass) have a larger probability of escaping the cluster intact. These results help us to obtain a better understanding of the difference between the observed fractions of exoplanets-hosting stars in star clusters and in the Galactic field. It also allows us to make predictions about the free-floating planet population over time in different stellar environments.

show abstract

Dynamical Interactions Make Hot Jupiters in Open Star Clusters

Cited by 84 publications

References 54 publications

Search for giant planets in M67

Search for giant planets in M67

The GAPS programme with HARPS-N at TNG

The dynamical fate of planetary systems in young star clusters

Contact Info

Product

Resources

About