GW Ori: circumtriple rings and planets

Smallwood, Jeremy L.; Nealon, Rebecca; Chen, Cheng; Martin, Rebecca G.; Bi, Jiaqing; Dong, Ruobing; Pinte, C.

doi:10.1093/mnras/stab2624

Cited by 18 publications

(9 citation statements)

References 107 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…( 2) in Facchini et al 2018). In fact, Smallwood et al (2021) carried out smoothed particle hydrodynamics (SPH) simulations with varying viscosities in the disk and found no breaking in the bending-wave regime. They suggest instead that the stellar multiple leads to a warped inner disk after a planet carved a gap in the disk.…”

Section: Observations Of Misaligned Configurationsmentioning

confidence: 99%

Misaligned disks induced by infall

Küffmeier

Dullemond

Reißl

et al. 2021

A&A

View full text Add to dashboard Cite

Arc- and tail-like structures associated with disks around Herbig stars can be a consequence of infall events occurring after the initial collapse phase of a forming star, consistent with the observation of luminosity bursts. An encounter event of gas with an existing star can lead to the formation of a second-generation disk significantly after the initial protostellar collapse phase. Additionally, observations of shadows in disks can be well described by a configuration of a misaligned inner and outer disk, such that the inner disk casts a shadow on the outer disk. Carrying out altogether eleven 3D hydrodynamical models with the moving mesh code AREPO, we tested whether a late encounter of an existing star–disk system with a cloudlet of gas can lead to the formation of an outer disk that is misaligned with respect to the primordial inner disk. Our models demonstrate that a second-generation disk with a large misalignment with respect to an existing primordial disk can easily form if the infall angle is large. The second-generation outer disk is more eccentric, though the asymmetric infall also triggers eccentricity of the inner disk of e ≈ 0.05 to 0.1. Retrograde infall can lead to the formation of counter-rotating disks and enhanced accretion. As the angular momentum of the inner disk is reduced, the inner disk shrinks and a gap forms between the two disks. The resulting misaligned disk system can survive for ~100 kyr or longer without aligning with each other even for low primordial disk masses given an infall mass of ~10−4 M⊙. A synthetic image for one of our models reveals shadows in the outer disk similar to the ones observed in multiple transition disks that are caused by the misaligned inner disk. We conclude that late infall onto an existing star–disk system leads to the formation of a misaligned outer disk for infall that is inclined with respect to the orientation of the inner disk. Infall might therefore be responsible for observations of shadows in at least some transition disks.

show abstract

Section: Observations Of Misaligned Configurationsmentioning

confidence: 99%

Misaligned disks induced by infall

Küffmeier

Dullemond

Reißl

et al. 2021

A&A

View full text Add to dashboard Cite

show abstract

“…There are two triple star systems that may have planets orbiting them, GG Tauri A (Phuong et al 2020b) and GW Ori (Bi et al 2020;Smallwood et al 2021). The GG Tauri A system consists of three stars (Di Folco et al 2014) with m B = 0.6 M e , m Aa = 0.38 M e , and m Ab = 0.3 M e .…”

Section: Discussionmentioning

confidence: 99%

“…Multiple stellar systems are common in star-forming regions (Duchêne & Kraus 2013). Disks around triple star systems are also expected to be common (Tobin et al 2016;Bate 2018), and there are several well-known examples including GG Tauri A (Di Folco et al 2014;Keppler et al 2020;Phuong et al 2020a) and GW Ori (Bi et al 2020;Kraus et al 2020;Smallwood et al 2021). A common feature of these disks is that they are tilted with respect to the orbital plane of the stars.…”

Section: Introductionmentioning

confidence: 99%

Polar Circumtriple Planets and Disks Can Only Form Close to a Triple Star

Lepp

Martin

Lubow

2023

ApJL

Self Cite

View full text Add to dashboard Cite

Observations of protoplanetary disks around binary and triple star systems suggest that misalignments between the orbital plane of the stars and the disks are common. Motivated by recent observations of polar circumbinary disks, we explore the possibility of polar circumtriple disks and therefore polar circumtriple planets that could form in such a disk. With n-body simulations and analytic methods, we find that the inclusion of a third star, and the associated apsidal precession, significantly reduces the radial range of polar orbits so that circumtriple polar disks and planets can only be found close to the stellar system. Outside of a critical radius that is typically in the range of 3–10 times the outer binary separation, depending upon the binary parameters, the orbits behave the same as they do around a circular orbit binary. For some observed systems that have shorter-period inner binaries, the critical radius is considerably larger. If polar circumtriple planets can form, we suggest that it is likely that they form in a disk that was subject to breaking.

show abstract

“…The data also indicate complex disk dynamics initiated by the various stellar components. Subsequent work by Smallwood et al (2021) conveyed evidence of disk breaking that, according to the authors, is likely caused by undetected planets, which, if confirmed, would constitute the first planet(s) identified in a circumtriple orbit.…”

Section: Introductionmentioning

confidence: 99%

An Early Catalog of Planet-hosting Multiple-star Systems of Order Three and Higher

Cuntz

Luke

Millard

et al. 2022

ApJS

View full text Add to dashboard Cite

We present a catalog (status 2022 July 1) of triple and higher-order systems identified containing exoplanets based on data from the literature, including various analyses. We explore statistical properties of the systems with a focus on both the stars and the planets. So far, about 30 triple systems and one to three quadruple systems, including (mildly) controversial cases, have been found. The total number of planets is close to 40. All planet-hosting triple-star systems are highly hierarchic, consisting of a quasi-binary complemented by a distant stellar component, which is in orbit about the common center of mass. Furthermore, the quadruple systems are in fact pairs of close binaries (“double–doubles”), with one binary harboring a planet. For the different types of star–planet systems, we introduce a template for the classifications of planetary orbital configurations in correspondence to the hierarchy of the system and the planetary host. The data show that almost all stars are main-sequence stars, as expected. However, the stellar primaries tend to be more massive (i.e., corresponding to spectral types A, F, and G) than expected from single-star statistics, a finding also valid for stellar secondaries but less pronounced. Tertiary stellar components are almost exclusively low-mass stars of spectral type M. Almost all planets have been discovered based on either the Radial Velocity method or the Transit method. Both gas giants (the dominant type) and terrestrial planets (including super-Earths) have been identified. We anticipate the expansion of this database in the light of future planetary search missions.

show abstract

GW Ori: circumtriple rings and planets

Cited by 18 publications

References 107 publications

Misaligned disks induced by infall

Misaligned disks induced by infall

Polar Circumtriple Planets and Disks Can Only Form Close to a Triple Star

An Early Catalog of Planet-hosting Multiple-star Systems of Order Three and Higher

Contact Info

Product

Resources

About