Multi-wavelength observations of the young binary system Haro 6-10: The case of misaligned discs

Roccatagliata, V.; Ratzka, Thorsten; Henning, Th.; Wolf, S.; Leinert, Christoph; Bouwman, J.

doi:10.1051/0004-6361/201116805

Cited by 31 publications

(47 citation statements)

References 66 publications

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“…Polarimetry can also be used to study disc alignment (Monin et al 1998;Jensen et al 2004;Wolf et al 2001;Monin et al 2006). However, we now have a growing list of directly imaged misaligned discs in wide ( ∼ > 100 au) Class II systems (Koresko 1998;Stapelfeldt et al 1998;Kang et al 2008;Ratzka et al 2009;Roccatagliata et al 2011;Jensen & Akeson 2014;Salyk et al 2014;Williams et al 2014), including the recently observed system Ophiuchus SR24 that appears to have two discs misaligned by ≈ 108…”

Section: Misaligned Circumstellar Discs In Multiple Systemsmentioning

confidence: 99%

On the diversity and statistical properties of protostellar discs

Bate

2018

Monthly Notices of the Royal Astronomical Society

287

320

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We present results from the first population synthesis study of protostellar discs. We analyse the evolution and properties of a large sample of protostellar discs formed in a radiation hydrodynamical simulation of star cluster formation. Due to the chaotic nature of the star formation process, we find an enormous diversity of young protostellar discs, including misaligned discs, and discs whose orientations vary with time. Star-disc interactions truncate discs and produce multiple systems. Discs may be destroyed in dynamical encounters and/or through ram-pressure stripping, but reform by later gas accretion. We quantify the distributions of disc mass and radii for protostellar ages up to ≈ 10 5 yrs. For low-mass protostars, disc masses tend to increase with both age and protostellar mass. Disc radii range from of order ten to a few hundred au, grow in size on timescales ∼ < 10 4 yr, and are smaller around lower-mass protostars. The radial surface density profiles of isolated protostellar discs are flatter than the minimum mass solar nebula model, typically scaling as Σ ∝ r −1. Disc to protostar mass ratios rarely exceed two, with a typical range of M d /M * = 0.1−1 to ages ∼ < 10 4 yrs and decreasing thereafter. We quantify the relative orientation angles of circumstellar discs and the orbit of bound pairs of protostars, finding a preference for alignment that strengths with decreasing separation. We also investigate how the orientations of the outer parts of discs differ from the protostellar and inner disc spins for isolated protostars and pairs.

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Section: Misaligned Circumstellar Discs In Multiple Systemsmentioning

confidence: 99%

On the diversity and statistical properties of protostellar discs

Bate

2018

Monthly Notices of the Royal Astronomical Society

287

320

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“…The circumstellar disks are misaligned and the system is embedded in a common envelope (Roccatagliata et al 2011). H 2 O maser emission has been recently reported, and suggest that the Southern component is itself a close binary (Wilking et al 2012).…”

Section: Appendix A: Comments On Individual Sourcesmentioning

confidence: 99%

A sensitive survey for¹³CO, CN, H₂CO, and SO in the disks of T Tauri and Herbig Ae stars

Guilloteau¹,

Folco²,

Dutrey³

et al. 2013

A&A

104

151

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Aims. We investigate the suitability of several molecular tracers, in particular CN N = 2−1 line emission, as a confusion-free probe of the kinematics of circumstellar disks. Methods. We use the IRAM 30-m telescope to perform a sensitive search for CN N = 2−1 in 42 T Tauri or Herbig Ae systems located principally in the Taurus-Auriga region. 13 CO J = 2−1 is observed simultaneously to provide an indication of the level of confusion with the surrounding molecular cloud. The bandpass also contains two transitions of ortho-H 2 CO, one of SO and the C 17 O J = 2−1 line which provide complementary information on the nature of the emission. Results. While 13 CO is in general dominated by residual emission from the cloud, CN exhibits a high disk detection rate >50% in our sample. We even report CN detection in stars for which interferometric searches failed to detect 12 CO, presumably because of obscuration by a foreground, optically thick, cloud. Comparison between CN and o-H 2 CO or SO line profiles and intensities divide the sample in two main categories. Sources with SO emission are bright and have strong H 2 CO emission, leading in general to [H 2 CO/CN] > 0.5. Furthermore, their line profiles, combined with a priori information on the objects, suggest that the emission is coming from outflows or envelopes rather than from a circumstellar disk. On the other hand, most sources have [H 2 CO/CN] < 0.3, no SO emission, and some of them exhibit clear double-peaked profiles characteristics of rotating disks. In this second category, CN is likely tracing the proto-planetary disks. From the line flux and opacity derived from the hyperfine ratios, we constrain the outer radii of the disks, which range from 300 to 600 AU. The overall gas disk detection rate (including all molecular tracers) is ∼68%, and decreases for fainter continuum sources. Conclusions. The current study demonstrates that gas disks, like dust disks, are ubiquitous around young PMS stars in regions of isolated star formation, and that a large fraction of them have R out > ∼ 300 AU. It also shows the potential of the CN N = 2−1 transition to probe the kinematics of these disks, thereby measuring the stellar mass, using high resolution observations with ALMA.

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“…However, the multi-epoch Spitzer data do not show significant mid-infrared variation on timescales of a few months up to a few years, in contrast with the near-infrared ground-based results and with IRS 46. The mid-infrared continuum of GV Tau N is about an order of magnitude brighter than the continuum of GV Tau S between 8−13 μm (Przygodda 2004;Roccatagliata et al 2011). Since no absorption was seen in GV Tau S in Gibb et al (2007) and Doppmann et al (2008) it is assumed that the majority of the absorption arises toward GV Tau N. However, the continuum emission from the southern source captured in the Spitzer-IRS aperture slightly reduces the total optical depth of the absorption lines in the spectrum.…”

Section: Irs 46 and Gv Taumentioning

confidence: 99%

Exploring organic chemistry in planet-forming zones

Bast

Lahuis

Dishoeck

et al. 2013

A&A

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Context. Over the last few years, the chemistry of molecules other than CO in the planet-forming zones of disks is starting to be explored with Spitzer and high-resolution ground-based data. However, these studies have focused only on a few simple molecules. Aims. The aim of this study is to put observational constraints on the presence of more complex organic and sulfur-bearing molecules predicted to be abundant in chemical models of disks and to simulate high resolution spectra in view of future missions. Methods. High signal-to-noise ratio (S/N) Spitzer spectra of the near edge-on disks IRS 46 and GV Tau are used to search for midinfrared absorption bands of various molecules. These disks are good laboratories because absorption studies do not suffer from low line/continuum ratios that plague emission data. Simple local thermodynamic equilibrium (LTE) slab models are used to infer column densities (or upper limits) and excitation temperatures. Results. Mid-infrared bands of HCN, C 2 H 2 and CO 2 are clearly detected toward both sources. The HCN and C 2 H 2 absorption arises in warm gas with excitation temperatures of 400−700 K, whereas the CO 2 absorption originates in cooler gas of ∼250 K. Column densities and their ratios are comparable for the two sources. No other absorption features are detected at the 3σ level. Column density limits of the majority of molecules predicted to be abundant in the inner disk -C 2 H 4 , C 2 H 6 , C 6 H 6 , C 3 H 4 , C 4 H 2 , CH 3 , HNC, HC 3 N, CH 3 CN, NH 3 and SO 2 -are determined and compared with disk models. Conclusions. The inferred abundance ratios and limits with respect to C 2 H 2 and HCN are roughly consistent with models of the chemistry in high temperature gas. Models of UV irradiated disk surfaces generally agree better with the data than pure X-ray models. The limit on NH 3 /HCN implies that evaporation of NH 3 -containing ices is only a minor contributor. The inferred abundances and their limits also compare well with those found in comets, suggesting that part of the cometary material may derive from warm inner disk gas. The high resolution simulations show that future instruments on the James Webb Space Telescope (JWST), the Extremely Large Telescopes (ELTs), the Stratospheric Observatory for Infrared Astronomy (SOFIA) and the Space Infrared Telescope for Cosmology and Astrophysics (SPICA) can probe up to an order of magnitude lower abundance ratios and put important new constraints on the models, especially if pushed to high S/Ns.

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Multi-wavelength observations of the young binary system Haro 6-10: The case of misaligned discs

Cited by 31 publications

References 66 publications

On the diversity and statistical properties of protostellar discs

On the diversity and statistical properties of protostellar discs

A sensitive survey for¹³CO, CN, H₂CO, and SO in the disks of T Tauri and Herbig Ae stars

Exploring organic chemistry in planet-forming zones

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Multi-wavelength observations of the young binary system Haro 6-10: The case of misaligned discs

Cited by 31 publications

References 66 publications

On the diversity and statistical properties of protostellar discs

On the diversity and statistical properties of protostellar discs

A sensitive survey for13CO, CN, H2CO, and SO in the disks of T Tauri and Herbig Ae stars

Exploring organic chemistry in planet-forming zones

Contact Info

Product

Resources

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A sensitive survey for¹³CO, CN, H₂CO, and SO in the disks of T Tauri and Herbig Ae stars