La Ronde

Dvorak, Paul; Schnitzler, Alfons; Frank, Stephanie; Marcus, Jacqueline; Marcus, Frank I.

doi:10.2307/327465

Cited by 11 publications

(11 citation statements)

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“…The planet is an S-type (satellite) planet, meaning that it orbits one component of a stellar multiple system (Dvorak 1982). Most of the literature on planets in multiple star systems considers planets in binary systems with solar-type primary stars (Eggenberger 2010;Wang et al 2014aWang et al , 2014bWinn & Fabrycky 2015;Kraus et al 2016;Matson et al 2018).…”

Section: Discussionmentioning

confidence: 99%

Three Red Suns in the Sky: A Transiting, Terrestrial Planet in a Triple M-dwarf System at 6.9 pc

Winters

Medina

Irwin

et al. 2019

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We present the discovery from Transiting Exoplanet Survey Satellite (TESS) data of LTT1445Ab. At a distance of 6.9 pc, it is the second nearest transiting exoplanet system found to date, and the closest one known for which the primary is an M dwarf. The host stellar system consists of three mid-to-late M dwarfs in a hierarchical configuration, which are blended in one TESSpixel. We use MEarth data and results from the Science Processing Operations Center data validation report to determine that the planet transits the primary star in the system. The planet has a radius of-+ 1.38 0.12 0.13 Å R , an orbital period of-+ 5.35882 0.00031 0.00030 days, and an equilibrium temperature of-+ 433 27 28 K. With radial velocities from the High Accuracy Radial Velocity Planet Searcher, we place a 3σ upper mass limit of 8.4 Å M on the planet. LTT1445Ab provides one of the best opportunities to date for the spectroscopic study of the atmosphere of a terrestrial world. We also present a detailed characterization of the host stellar system. We use high-resolution spectroscopy and imaging to rule out the presence of any other close stellar or brown dwarf companions. Nineteen years of photometric monitoring of A and BC indicate a moderate amount of variability, in agreement with that observed in the TESSlight-curve data. We derive a preliminary astrometric orbit for the BC pair that reveals an edge-on and eccentric configuration. The presence of a transiting planet in this system hints that the entire system may be co-planar, implying that the system may have formed from the early fragmentation of an individual protostellar core.

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Section: Discussionmentioning

confidence: 99%

Three Red Suns in the Sky: A Transiting, Terrestrial Planet in a Triple M-dwarf System at 6.9 pc

Winters

Medina

Irwin

et al. 2019

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“…Circumbinary planets (hereafter, CBPs), i.e., planets that orbit an entire binary star system, can reveal their presence in a variety of different ways. Known as P-type systems (Dvorak 1982), these planets, if sufficiently large, may affect radial velocities of the stars or the timing of stellar eclipses (Schwarz et al 2011). Several claims of the detection of CBPs using eclipse timing variations have been made (for example Qian et al 2012aQian et al ,b, 2013Lee et al 2014), but, the validity of these detections is currently under question (e.g., Marsh 2018).…”

Section: Introductionmentioning

confidence: 99%

Discovery of a Third Transiting Planet in the Kepler-47 Circumbinary System

Orosz

Welsh

Haghighipour

et al. 2019

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Of the nine confirmed transiting circumbinary planet systems, only Kepler-47 is known to contain more than one planet. Kepler-47 b (the "inner planet") has an orbital period of 49.5 days and a radius of about 3 R ⊕ . Kepler-47 c (the "outer planet") has an orbital period of 303.2 days and a radius of about 4.7 R ⊕ . Here we report the discovery of a third planet, Kepler-47 d (the "middle planet"), which has an orbital period of 187.4 days and a radius of about 7 R ⊕ . The presence of the middle planet allows us to place much better constraints on the masses of all three planets, where the 1σ ranges are less than 26 M ⊕ , between 7 − 43 M ⊕ , and between 2 − 5 M ⊕ for the inner, middle, and outer planets, respectively. The middle and outer planets have low bulk densities,

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“…Previously, Dvorak (1982) introduced the terminology of S-type and P-type orbits for system planets, which is now widely used by the orbital stability, planetary, and the astrobiology science communities. Evidently, besides the assessment of orbital stability behaviors, these terms are also appropriate for classifying binary system RHZs, if they exist.…”

Section: Proposed Habitability Classification: Habitability Types S mentioning

confidence: 99%

“…From the viewpoint of orbital mechanics, there are two different kinds of possible orbits (notwithstanding positions near the Lagrangian points L 4 and L 5 ) for planets in binary systems: S-type and P-type orbits (Dvorak 1982). A P-type orbit is attributed when the planet orbits both binary components, whereas in the case of an S-type orbit, the planet orbits only one of the binary components with the second component behaving as a perturbator.…”

Section: Introductionmentioning

confidence: 99%

Crystallographic and Dielectric Studies in the Solid Solution System PbCo_1/2W_1/2O₃–PbYb_1/2Ta_1/2O₃

Park¹,

Knowles²

1998

Jpn. J. Appl. Phys.

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A comprehensive approach is provided for the study of both S-type and P-type habitability in stellar binary systems, which in principle can also be expanded to systems of higher order. P-type orbits occur when the planet orbits both binary components, whereas in the case of S-type orbits, the planet orbits only one of the binary components with the second component considered a perturbator. The selected approach encapsulates a variety of different aspects, which include: (1) the consideration of a joint constraint, including orbital stability and a habitable region for a putative system planet through the stellar radiative energy fluxes ("radiative habitable zone"; RHZ), needs to be met; (2) the treatment of conservative, general, and extended zones of habitability for the various systems as defined for the solar system and beyond; (3) the provision of a combined formalism for the assessment of both S-type and P-type habitability; in particular, mathematical criteria are presented for the kind of system in which S-type and P-type habitability is realized; (4) applications of the attained theoretical approach to standard (theoretical) main-sequence stars. In principle, five different cases of habitability are identified, which are S-type and P-type habitability provided by the full extent of the RHZs; habitability, where the RHZs are truncated by the additional constraint of planetary orbital stability (referred to as ST-and PT-type, respectively); and cases of no habitability at all. Regarding the treatment of planetary orbital stability, we utilize the formulae of Holman & Wiegert as also used in previous studies. In this work, we focus on binary systems in circular orbits. Future applications will also consider binary systems in elliptical orbits and provide thorough comparisons to other methods and results given in the literature.

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La Ronde

Cited by 11 publications

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Three Red Suns in the Sky: A Transiting, Terrestrial Planet in a Triple M-dwarf System at 6.9 pc

Three Red Suns in the Sky: A Transiting, Terrestrial Planet in a Triple M-dwarf System at 6.9 pc

Discovery of a Third Transiting Planet in the Kepler-47 Circumbinary System

Crystallographic and Dielectric Studies in the Solid Solution System PbCo_1/2W_1/2O₃–PbYb_1/2Ta_1/2O₃

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La Ronde

Cited by 11 publications

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Three Red Suns in the Sky: A Transiting, Terrestrial Planet in a Triple M-dwarf System at 6.9 pc

Three Red Suns in the Sky: A Transiting, Terrestrial Planet in a Triple M-dwarf System at 6.9 pc

Discovery of a Third Transiting Planet in the Kepler-47 Circumbinary System

Crystallographic and Dielectric Studies in the Solid Solution System PbCo1/2W1/2O3–PbYb1/2Ta1/2O3

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Crystallographic and Dielectric Studies in the Solid Solution System PbCo_1/2W_1/2O₃–PbYb_1/2Ta_1/2O₃