A Pair of Warm Giant Planets near the 2:1 Mean Motion Resonance around the K-dwarf Star TOI-2202*

Abstract TOI-2202 b is a transiting warm Jovian-mass planet with an orbital period of P = 11.91 days identified from the Full Frame Images data of five different sectors of the TESS mission. Ten TESS transits of TOI-2202 b combined with three follow-up light curves obtained with the CHAT robotic telescope show strong transit timing variations (TTVs) with an amplitude of about 1.2 hr. Radial velocity follow-up with FEROS, HARPS, and PFS confirms the planetary nature of the transiting candidate (a b = 0.096 ± 0.001 au, m b = 0.98 ± 0.06 M Jup), and a dynamical analysis of RVs, transit data, and TTVs points to an outer Saturn-mass companion (a c = 0.155 ± 0.002 au, m c = 0.37 ± 0.10 M Jup) near the 2:1 mean motion resonance. Our stellar modeling indicates that TOI-2202 is an early K-type star with a mass of 0.82 M ⊙, a radius of 0.79 R ⊙, and solar-like metallicity. The TOI-2202 system is very interesting because of the two warm Jovian-mass planets near the 2:1 mean motion resonance, which is a rare configuration, and their formation and dynamical evolution are still not well understood.

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Capture and migration of Jupiter and Saturn in mean motion resonance in a gaseous protoplanetary disc

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/staa260 ◽

2020 ◽

Vol 492 (4) ◽

pp. 6007-6018 ◽

Cited By ~ 3

Author(s):

Raúl O Chametla ◽

Gennaro D’Angelo ◽

Mauricio Reyes-Ruiz ◽

F Javier Sánchez-Salcedo

Keyword(s):

Solar Nebula ◽

Dynamical Evolution ◽

Giant Planets ◽

Orbital Dynamics ◽

Evolutionary Path ◽

Mean Motion ◽

Evolutionary Scenario ◽

Low Probability ◽

And Migration ◽

Mean Motion Resonance

ABSTRACT We study the dynamical evolution of Jupiter and Saturn embedded in a gaseous, solar nebula-type disc by means of hydrodynamics simulations with the fargo2d1d code. We study the evolution for different initial separations of the planets’ orbits, ΔaSJ, to investigate whether they become captured in mean motion resonance (MMR) and the direction of the subsequent migration of the planet (inwards or outwards). We also provide an assessment of the planet’s orbital dynamics at different epochs of Saturn’s growth. We find that the evolution of initially compact orbital configurations is dependent on the value of ΔaSJ. This implies that an evolution as that proposed in the Grand Tack model depends on the precise initial orbits of Jupiter and Saturn and on the time-scales for their formation. Capture in the 1:2 MMR and inward or (nearly) stalled migration are highly favoured. Within its limits, our work suggests that the reversed migration, associated with the resonance capture of Jupiter and Saturn, may be a low-probability evolutionary scenario, so that other planetary systems with giant planets are not expected to have experienced a Grand Tack-like evolutionary path.

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A resonant pair of warm giant planets revealed by TESS

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/stz1141 ◽

2019 ◽

Vol 486 (4) ◽

pp. 4980-4986 ◽

Cited By ~ 5

Author(s):

David Kipping ◽

David Nesvorný ◽

Joel Hartman ◽

Guillermo Torres ◽

Gaspar Bakos ◽

...

Keyword(s):

Giant Planets ◽

Dynamical Model ◽

First Year ◽

Mean Motion ◽

M Dwarf ◽

Mean Motion Resonance ◽

Dynamical Masses

ABSTRACT We present the discovery of a pair of transiting giant planets using four sectors of TESS photometry. TOI-216 is a 0.87 M⊙ dwarf orbited by two transiters with radii of 8.2 and 11.3 R⊕, and periods of 17.01 and 34.57 d, respectively. Anticorrelated TTVs are clearly evident indicating that the transiters orbit the same star and interact via a near 2:1 mean motion resonance. By fitting the TTVs with a dynamical model, we infer masses of $30_{-14}^{+20}$ and $200_{-100}^{+170}$ M⊕, establishing that the objects are planetary in nature and have likely sub-Kronian and Kronian densities. TOI-216 lies close to the southern ecliptic pole and thus will be observed by TESS throughout the first year, providing an opportunity for continuous dynamical monitoring and considerable refinement of the dynamical masses presented here. TOI-216 closely resembles Kepler-9 in architecture, and we hypothesize that in such systems these Saturn analogues failed to fully open a gap and thus migrated far deeper into the system before becoming trapped into resonance, which would imply that future detections of new analogues may also have sub-Jupiter masses.

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The photometric follow-up observations for transiting exoplanet XO-2b

Proceedings of the International Astronomical Union ◽

10.1017/s1743921311020643 ◽

2010 ◽

Vol 6 (S276) ◽

pp. 426-427

Author(s):

Sheng-hong Gu ◽

Andrew Collier Cameron ◽

Xiao-bin Wang ◽

Xiang-song Fang ◽

Dong-tao Cao ◽

...

Keyword(s):

Orbital Period ◽

Light Curves ◽

Mcmc Algorithm ◽

System Parameters

AbstractFour new transit light curves of XO-2b obtained in 2008 and 2009, are analyzed by using MCMC algorithm, and the system parameters are derived. The result demonstrates that the orbital period of the system obtained from new observations is almost the same as Burke et al.'s one (2007), which does not confirm the result of Fernandez et al. (2009).

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Exploring the 7:4 mean motion resonance—I: Dynamical evolution of classical transneptunian objects

Planetary and Space Science ◽

10.1016/j.pss.2004.12.015 ◽

2005 ◽

Vol 53 (11) ◽

pp. 1175-1187 ◽

Cited By ~ 13

Author(s):

Patryk Sofia Lykawka ◽

Tadashi Mukai

Keyword(s):

Dynamical Evolution ◽

Mean Motion ◽

Transneptunian Objects ◽

Mean Motion Resonance

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Robotic Monitoring of Gravitationally Lensed Quasars

Advances in Astronomy ◽

10.1155/2010/347935 ◽

2010 ◽

Vol 2010 ◽

pp. 1-7 ◽

Cited By ~ 3

Author(s):

Luis J. Goicoechea ◽

Vyacheslav N. Shalyapin ◽

Aurora Ullán

Keyword(s):

Light Curves ◽

Current Status ◽

Second Phase ◽

Scientific Results ◽

Robotic Telescope

We report on the first observational phase of the Liverpool Quasar Lens Monitoring (LQLM) project. This mainly consisted of the optical follow-up of three lensed quasars using the 2 m Liverpool Robotic Telescope. The observational subprogram started in January 2005 and was completed in July 2007. We also describe our photometric approaches (including two pipelines to extract accurate and reliable fluxes of images of lensed quasars), the performance of the telescope when taking modest nightly exposures of lens systems, and the main scientific results from the observed light curves. The LQLM archive and the current status of the project (second phase) are also outlined.

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What to Expect from Transiting Multiplanet Systems

Proceedings of the International Astronomical Union ◽

10.1017/s1743921308026380 ◽

2008 ◽

Vol 4 (S253) ◽

pp. 173-179 ◽

Cited By ~ 2

Author(s):

Daniel C. Fabrycky

Keyword(s):

Radial Velocity ◽

Transit Time ◽

Dynamical Evolution ◽

Velocity Measurements ◽

Search Methods ◽

Tidal Evolution ◽

Transiting Planets ◽

Mean Motion ◽

Time Variations ◽

Mean Motion Resonance

AbstractSo far radial velocity measurements have discovered ~25 stars to host multiple planets. The statistics imply that many of the known hosts of transiting planets should have additional planets, yet none have been solidly detected. They will be soon, via complementary search methods of RV, transit-time variations of the known planet, and transits of the additional planet. When they are found, what can transit measurements add to studies of multiplanet dynamical evolution? First, mutual inclinations become measurable, for comparison to the solar system's disk-like configuration. Such measurements will give important constraints to planet-planet scattering models, just as the radial velocity measurements of eccentricity have done. Second, the Rossiter-McLaughlin effect measures stellar obliquity, which can be modified by two-planet dynamics with a tidally evolving inner planet. Third, transit-time variations are exquisitely sensitive to planets in mean motion resonance. Two planets differentially migrating in the disk can establish such resonances, and tidal evolution of the planets can break them, so the configuration and frequency of these resonances as a function of planetary parameters will constrain these processes.

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Formation and transformation of the 3:1 mean-motion resonance in 55 Cancri System

Proceedings of the International Astronomical Union ◽

10.1017/s1743921308017006 ◽

2007 ◽

Vol 3 (S249) ◽

pp. 485-490 ◽

Cited By ~ 1

Author(s):

Li-Yong Zhou ◽

Sylvio Ferraz-Mello ◽

Yi-Sui Sun

Keyword(s):

Configuration Space ◽

Rate Increase ◽

Dynamical Evolution ◽

Resonance Capture ◽

Resonance System ◽

Mean Motion ◽

Damping Rate ◽

Orbital Configuration ◽

Planetary Migration ◽

Mean Motion Resonance

AbstractWe report in this paper the numerical simulations of the capture into the 3:1 mean-motion resonance between the planets b and c in the 55 Cancri system. The results show that this resonance can be obtained by a differential planetary migration. The moderate initial eccentricities, relatively slower migration and suitable eccentricity damping rate increase significantly the probability of being trapped in this resonance. Otherwise, the system crosses the 3:1 commensurability avoiding resonance capture, to be eventually captured into a 2:1 resonance or some other higher-order resonances. After capture into resonance, the system can jump from one orbital configuration to another one if the migration continues, making a large region of the configuration space accessible for a resonance system. These investigations help us understand the diversity of resonance configurations and put some constraints on the early dynamical evolution of orbits in the extra-solar planetary systems.

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

Astronomy and Astrophysics ◽

10.1051/0004-6361/202038967 ◽

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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Co-ordinated Follow-Up of Transiting Planet Candidates with Robotic Telescope Facilities

Proceedings of the International Astronomical Union ◽

10.1017/s174392130802680x ◽

2008 ◽

Vol 4 (S253) ◽

pp. 412-415

Author(s):

R. A. Street ◽

T. A. Lister

Keyword(s):

False Alarm ◽

False Alarm Rate ◽

False Positives ◽

Light Curves ◽

Robotic Telescope ◽

High False Alarm Rate ◽

Planetary Transits

AbstractThere are now several large photometric surveys scanning millions of stellar light-curves for signs of planetary transits. All produce large candidate lists with a high false alarm rate, so that further observations are required to confirm new detections. One such survey, SuperWASP, produced ~150 candidates during the 2007–2008 season. Here we describe our campaign to follow-up 86 of these candidates using the robotic facilities of Las Cumbres Observatory Global Telescope Network and the Tenagra-II robotic telescope in Arizona. The aim of these observations was to eliminate false positives as far as possible ahead of spectroscopic follow-up and to provide additional photometry to help characterise the surviving targets.

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