Grid-based simulations of polar circumbinary discs: polar alignment and vortex formation

Rabago, Ian; Zhu, Zhaohuan; Martin, Rebecca G.; Lubow, Stephen H.

doi:10.1093/mnras/stad242

Cited by 9 publications

(4 citation statements)

References 85 publications

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“…An example of such objects is CQ Tau that additionally shows strong photometric variability at IR wavelengths (Hammond et al 2022). All features -spirals, shadows and asymmetries -could be signatures of binaries and their detection supports the scenario that these disks may host yet-undetected stellar companions (Ragusa et al 2017(Ragusa et al , 2020Calcino et al 2019;Rabago et al 2023). However, none of these stellar companions were found to date, and models including giant planets on eccentric orbits can also reproduce some of these features (Baruteau et al 2019;Calcino et al 2020;Pinilla et al 2022), so several scenarios remain viable.…”

Section: Non-detections Of Companions In Four Transition Disksmentioning

confidence: 73%

Searching for low-mass companions at small separations in transition disks with aperture masking interferometry

Stolker,

Kammerer,

Benisty

et al. 2024

A&A

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Transition disks have large central cavities that have been resolved by imaging surveys during recent years. Cavities and other substructures in circumstellar disks are often interpreted as signposts to massive companions. Detecting companions at small angular separations is challenging with coronagraphic imaging observations. We aim to search for stellar and substellar companions in the central regions of transition disks. Such companions could be responsible for the large dust-depleted cavities. We want to determine if these disks might be circumbinary in their nature, similar to the HD\,142527 system. We observed four systems, HD\,100453, HD\,100546, HD\,135344\,B, and PDS\,70, with the sparse aperture masking mode of VLT/SPHERE, also leveraging the star-hopping method with the adaptive optics system. We extracted the complex visibilities and bispectra from the $H2$ and $H3$ imaging data. A binary model was fit to the closure phases to search for companions and estimate detection limits. For validation, we also analyzed four archival datasets of HD\,142527 and inferred the orbital elements and atmospheric parameters of its low-mass stellar companion. We have not detected any significant point sources in the four observed systems. With a contrast sensitivity of approx 0.004, we can rule out stellar companions down to approx 2 au and partially explore the substellar regime at separations gtrsim 3--5 au. The analysis of HD\,142527\,B revealed that its projected orbit is aligned with dust features in the extended inner disk and that the mutual inclination with the outer disk is close to coplanar for one of the two solutions. Atmospheric modeling confirms the low-gravity and slightly reddened spectral appearance ($ 3300$ K, $ 3.7$, and $A_V 0.7$). The inferred and derived bulk parameters ($ -0.65$, $M_ 0.4$ $M_ and $R_ 1.46$ $R_ are in agreement with dynamical constraints and evolutionary tracks. In contrast to HD\,142527, we find no evidence that a close-in stellar companion is responsible for the resolved disk features of HD\,100453, HD\,100546, HD\,135344\,B, and PDS\,70. Instead of a dynamical effect by a stellar companion, the formation of giant planets or even low-mass brown dwarfs could be shaping the innermost environment (lesssim 20 au) of these circumstellar disks, as is the case with the planetary system of PDS\,70.

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Section: Non-detections Of Companions In Four Transition Disksmentioning

confidence: 73%

Searching for low-mass companions at small separations in transition disks with aperture masking interferometry

Stolker,

Kammerer,

Benisty

et al. 2024

A&A

View full text Add to dashboard Cite

show abstract

“…In fact, the disk is close to alignment with the binary eccentricity vector, a configuration known as polar alignment (see the left panel of Figure 1). This is a stable state for a circumbinary disk around an eccentric binary (Aly et al 2015;Martin & Lubow 2017;Lubow & Martin 2018;Zanazzi & Lai 2018;Cuello & Giuppone 2019;Smallwood et al 2020;Rabago et al 2023). Previously, there have been observations of two polar aligned circumbinary gas disks (Kennedy et al 2019;Kenworthy et al 2022) and one debris disk (Kennedy et al 2012) around eccentric main-sequence star binaries.…”

Section: Introductionmentioning

confidence: 85%

“…We consider here a model in which the disk polar alignment in AC Her results from the evolution of an initially moderately misaligned disk to the polar orientation by means of the tidal evolution of a viscous disk (Aly et al 2015;Martin & Lubow 2017;Lubow & Martin 2018;Zanazzi & Lai 2018;Cuello & Giuppone 2019;Smallwood et al 2020;Rabago et al 2023). The application of this model imposes constraints of the origin and evolution of the circumbinary disk.…”

Section: Implications Of a Polar Aligned Diskmentioning

confidence: 99%

AC Her: Evidence of the First Polar Circumbinary Planet

Martin,

Lubow,

Vallet

et al. 2023

ApJL

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We examine the geometry of the post–asymptotic giant branch (AGB) star binary AC Her and its circumbinary disk. We show that the observations describe a binary orbit that is perpendicular to the disk with an angular momentum vector that is within 9° of the binary eccentricity vector, meaning that the disk is close to a stable polar alignment. The most likely explanation for the very large inner radius of the dust is a planet within the circumbinary disk. This is therefore both the first reported detection of a polar circumbinary disk around a post-AGB binary and the first evidence of a polar circumbinary planet. We consider the dynamical constraints on the circumbinary disk size and mass. The polar circumbinary disk feeds circumstellar disks with gas on orbits that are highly inclined with respect to the binary orbit plane. The resulting circumstellar disk inclination could be anywhere from coplanar to polar depending upon the competition between the mass accretion and binary torques.

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“…Theoretical studies have shown that misaligned disks can evolve either toward a coplanar alignment or a polar configuration around eccentric binaries (Aly et al 2015;Martin & Lubow 2017;Zanazzi & Lai 2018;Cuello & Giuppone 2019;Ceppi et al 2023;Rabago et al 2023). This is because particle orbits around an eccentric binary undergo nodal precession, either about the binary angular momentum vector (circulating orbits) or the stationary inclination (librating orbits), depending upon their initial inclination (Verrier & Evans 2009;Farago & Laskar 2010;Doolin & Blundell 2011;Naoz et al 2017;Chen et al 2019).…”

Section: Introductionmentioning

confidence: 99%

Relativistic Effects on Circumbinary Disk Evolution: Breaking the Polar Alignment around Eccentric Black Hole Binary Systems

Childs,

Martin,

Nixon

et al. 2024

ApJ

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We study the effects of general relativity (GR) on the evolution and alignment of circumbinary disks around binaries on all scales. We implement relativistic apsidal precession of the binary into the hydrodynamics code phantom. We find that the effects of GR can suppress the stable polar alignment of a circumbinary disk, depending on how the relativistic binary apsidal precession timescale compares to the disk nodal precession timescale. Studies of circumbinary disk evolution typically ignore the effects of GR, which is an appropriate simplification for low-mass or widely separated binary systems. In this case, polar alignment occurs, provided that the disks initial misalignment is sufficiently large. However, systems with a very short relativistic precession timescale cannot polar align and instead move toward coplanar alignment. In the intermediate regime where the timescales are similar, the outcome depends upon the properties of the disk. Polar alignment is more likely in the wavelike disk regime (where the disk viscosity parameter is less than the aspect ratio, α < H/r), since the disk is in good radial communication. In the viscous disk regime, disk breaking is more likely. Multiple rings can destructively interact with one another, resulting in short disk lifetimes and the disk moving toward coplanar alignment. Around main-sequence star or stellar mass black hole binaries, polar alignment may be suppressed far from the binary, but in general, the inner parts of the disk can align to polar. Polar alignment may be completely suppressed for disks around supermassive black holes for close binary separations.

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Grid-based simulations of polar circumbinary discs: polar alignment and vortex formation

Cited by 9 publications

References 85 publications

Searching for low-mass companions at small separations in transition disks with aperture masking interferometry

Searching for low-mass companions at small separations in transition disks with aperture masking interferometry

AC Her: Evidence of the First Polar Circumbinary Planet

Relativistic Effects on Circumbinary Disk Evolution: Breaking the Polar Alignment around Eccentric Black Hole Binary Systems

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