Misaligned Circumstellar Disks and Orbital Motion of the Young Binary XZ Tau

Ichikawa, Takanori; Kido, Miyu; Takaishi, Daisuke; Shimajiri, Yoshito; Tsukamoto, Yusuke; Takakuwa, Shigehisa

doi:10.3847/1538-4357/ac0dc3

Cited by 10 publications

(9 citation statements)

References 56 publications

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“…Qualitatively, the key difference between CBDs and circumstellar disks is that in former/latter, the binary torque is exerted at the inner/outer region of the disk, which contains small/larger amount of angular momentum, leading to relatively large/small warp and thus faster/slower viscous damping. Overall, these results are consistent with the observations that most CBDs are nearly coplanar with their host binaries (Czekala et al 2019), while circumstellar disks within young stellar binaries are often misaligned (e.g., Jensen & Akeson 2014, Ichikawa et al 2021.…”

Section: Disk Warping Breaking and Alignmentsupporting

confidence: 89%

Circumbinary Accretion: From Binary Stars to Massive Binary Black Holes

Dong¹,

Muñoz²

2022

Preprint

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We review recent works on the dynamics of circumbinary accretion, including time variability, angular momentum transfer between the disk and the binary, and the secular evolution of accreting binaries. These dynamics can impact stellar binary formation/evolution, circumbinary planet formation/migration, and the evolution of (super)massive black-hole binaries. We discuss the dynamics and evolution of inclined/warped circumbinary disks and connect with recent observations of protoplanetary disks. A special kind of circumbinary accretion involves binaries embedded in "big" disks, which may contribute to the mergers of stellar-mass black holes in AGN disks. Highlights include: Circumbinary accretion is highly variable, being modulated at P b (the binary period) or ∼ 5Pp, depending on the binary eccentricity e b and mass ratio q b . The inner region of the circumbinary disk can develop coherent eccentric structure, which may modulate the accretion and affect the physical processes (e.g. planet migration) taking place in the disk. Over long timescales, circumbinary accretion steers binaries toward equal masses, and it does not always lead to binary orbital decay, as is commonly assumed. The secular orbital evolution depends on the binary parameters (e b and q b ), and on the thermodynamic properties of the accreting gas. A misaligned disk around a low-eccentricity binary tends to evolve toward coplanarity due to viscous dissipation. But when e b is significant, the disk can evolve toward "polar alignment", with the disk plane perpendicular to the binary plane.

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Section: Disk Warping Breaking and Alignmentsupporting

confidence: 89%

Circumbinary Accretion: From Binary Stars to Massive Binary Black Holes

Dong¹,

Muñoz²

2022

Preprint

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“…Absolute proper motions can, in principle, inform us about the relative masses of the two components in the binary, since the center of mass is closer to the more massive component, and therefore this component is expected to be the one that shows smaller absolute proper motions. However, when the system has a significant overall proper motion, which is not independently known, as in our case, disentangling both types of motions becomes extremely challenging unless the data cover a significant fraction of the orbital period (e.g., in XZ Tau: Carrasco-González et al 2009;Ichikawa et al 2021). We note that measuring the difference in the absolute proper motions of the two components of the A1-A2 IRAS 16293 −2422 binary is insufficient to derive the relative masses and that resolved gas kinematics is required for this purpose (see Maureira et al 2020 for details).…”

Section: Proper Motionsmentioning

confidence: 96%

“…So far, only for a limited number of these systems there is available (but partial) observational information about their physical properties, such as temperatures, kinematics (from radial velocities and proper motions), presence of circumbinary disks, stellar and disk masses (from dust and molecular emission and from dynamics), chemical properties, and interaction with the surrounding medium (e.g., outflows and interaction with the ambient molecular cloud, flyby encounters, and tidal interaction with nearby young stars). Some examples where these studies have been performed are the binary systems L1551 IRS 5 (Rodríguez et al 1998;Cruz-Sáenz de Miera et al 2019;Takakuwa et al 2020), RW Aur (Cabrit et al 2006;Rodriguez et al 2018), L1551 NE (Takakuwa et al 2014(Takakuwa et al , 2017, XZ Tau (Carrasco-González et al 2009;Zapata et al 2015;Osorio et al 2016;Ichikawa et al 2021), GG Tau (Phuong et al 2020), BHB2007 (Alves et al 2019), UX Tau (Zapata et al 2020), and IRAS 16293−2422 (Maureira et al 2020).…”

Section: Introductionmentioning

confidence: 99%

The Physical Properties of the SVS 13 Protobinary System: Two Circumstellar Disks and a Spiraling Circumbinary Disk in the Making

Rodríguez¹,

Anglada²,

Blázquez-Calero³

et al. 2022

ApJ

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We present Very Large Array (VLA) and Atacama Large Millimeter/submillimeter Array (ALMA) observations of the close (0.″3 = 90 au separation) protobinary system SVS 13. We detect two small circumstellar disks (radii ∼12 and ∼9 au in dust, and ∼30 au in gas) with masses of ∼0.004–0.009 M ☉ for VLA 4A (the western component) and ∼0.009–0.030 M ☉ for VLA 4B (the eastern component). A circumbinary disk with prominent spiral arms extending ∼500 au and a mass of ∼0.052 M ☉ appears to be in the earliest stages of formation. The dust emission is more compact and with a very high optical depth toward VLA 4B, while toward VLA 4A the dust column density is lower, allowing the detection of stronger molecular transitions. We infer rotational temperatures of ∼140 K, on scales of ∼30 au, across the whole source, and a rich chemistry. Molecular transitions typical of hot corinos are detected toward both protostars, being stronger toward VLA 4A, with several ethylene glycol transitions detected only toward this source. There are clear velocity gradients, which we interpret in terms of infall plus rotation of the circumbinary disk, and pure rotation of the circumstellar disk of VLA 4A. We measured orbital proper motions and determined a total stellar mass of 1 M ☉. From the molecular kinematics, we infer the geometry and orientation of the system, and stellar masses of ∼0.26 M ☉ for VLA 4A and ∼0.60 M ☉ for VLA 4B.

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“…Such disks are interesting to study to test photoevaporation models, but also for possible small scale cavities carved by giant planets at small orbits of a few au which have formed in situ. The only small cavity transition disk candidates studied at high resolution to date are CX Tau (Facchini et al 2019) which did not reveal an inner cavity, the ISO-Oph 2 secondary with a 2.2 au inner cavity (González-Ruilova et al 2020) and XZ Tau B (Osorio et al 2016) which revealed an inner cavity of 1.3 au radius, but this was not recovered in later high resolution observations (Ichikawa et al 2021). Small inner cavities 10 au were resolved in millimeter images of Sz 129 and MHO 6, despite not showing any indication of a dip in the SED (Andrews et al 2018a;Kurtovic et al 2021).…”

Section: Introductionmentioning

confidence: 98%

High-resolution ALMA observations of transition disk candidates in Lupus

Marel¹,

Williams²,

Picogna³

et al. 2022

Preprint

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Context. Transition disks with small inner dust cavities are interesting targets for the study of disk clearing mechanisms. Such disks have been identified through a deficit in the infrared part of their SED, but spatially resolved millimeter imaging is required to confirm the presence of an inner dust cavity. Aims. The aim of this study is to image the millimeter-dust distribution of 10 transition disk candidates selected from both SED criteria and from tentative detections of inner cavities in low-resolution observations to verify their nature and to understand their origin. Methods. We use high-resolution ALMA observations of 30 mas resolution in Band 6 continuum and 12 CO 2-1 emission of 10 transition disk candidates in the Lupus star forming region, in order to confirm the presence of inner dust cavities and infer the responsible mechanism. The continuum data are analyzed using visibility modeling and the SEDs are compared with radiative transfer models.Results. Out of the six transition disk candidates selected from their SED, only one disk revealed an inner dust cavity of 4 au in radius. Three of the other disks are highly inclined, which limits the detectability of an inner dust cavity but it is also demonstrated to be the possible cause for the infrared deficit in their SED. The two remaining SED-selected disks are very compact, with dust radii of only ∼3 au. From the four candidates selected from low-resolution images, three new transition disks with large inner cavities >20 au are identified, bringing the total number of transition disks with large cavities in Lupus to 13. Conclusions. SED-selected transition disks with small cavities are biased towards highly inclined and compact disks, which casts doubt on the use of their occurence rates in estimating dispersal timescales of photoevaporation. Using newly derived disk dust masses and radii, we re-evaluate the size-luminosity and M dust − M star relations. These relations can be understood if the bright disks are dominated by disks with substructure whereas faint disks are dominated by drift-dominated disks.

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Misaligned Circumstellar Disks and Orbital Motion of the Young Binary XZ Tau

Cited by 10 publications

References 56 publications

Circumbinary Accretion: From Binary Stars to Massive Binary Black Holes

Circumbinary Accretion: From Binary Stars to Massive Binary Black Holes

The Physical Properties of the SVS 13 Protobinary System: Two Circumstellar Disks and a Spiraling Circumbinary Disk in the Making

High-resolution ALMA observations of transition disk candidates in Lupus

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