Constraining the wind launching region in Herbig Ae stars: AMBER/VLTI spectroscopy of HD 104237

Tatulli, E.; Isella, Andrea; Natta, A.; Testi, L.; Marconi, A.; Malbet, Fabien; Stee, Philippe; Petrov, R.; Millour, F.; Chelli, A.; Duvert, G.; Antonelli, P.; Beckmann, U.; Bresson, Y.; Dugué, M.; Gennari, S.; Glück, L.; Kern, P.; Lagarde, S.; Coarer, E. Le; Lisi, F.; Perraut, K.; Puget, P.; Rantakyrö, F.; Robbe-Dubois, S.; Roussel, Alain; Weigelt, G.; Zins, G.; Accardo, M.; Acke, B.; Agabi, Karim; Altariba, E.; Arezki, B.; Aristidi, Éric; Baffa, C.; Behrend, J.; Blöcker, T.; Bonhomme, S.; Busoni, S.; Cassaing, F.; Clausse, J. M.; Colin, J.; Connot, C.; Delboulbé, A.; Souza, A. Domiciano de; Driebe, T.; Feautrier, Philippe; Ferruzzi, D.; Forveille, T.; Fossat, E.; Foy, R.; Fraix-Burnet, Didier; Gallardo, Aurelio; Giani, E.; Gil, C.; Glentzlin, A.; Heiden, M.; Heininger, M.; Utrera, O. Hernández; Hofmann, Karl H.; Kamm, D.; Kiekebusch, M.; Kraus, Stefan; Contel, D. Le; Contel, J. M. Le; Lesourd, T.; López, B.; López, M.; Magnard, Y.; Mars, G.; Martinot-Lagarde, G.; Mathias, P.; Mège, P.; Monin, J.; Mouillet, D.; Mourard, D.; Nußbaum, E.; Ohnaka, K.; Pacheco, J. A. de Freitas; Perrier, C.; Rabbia, Yves; Rebattu, S.; Reynaud, François; Richichi, A.; Robini, A.; Sacchettini, M.; Schertl, D.; Schöller, M.; Solscheid, W.; Spang, A.; Stefanini, P.; Tallon, Michel; Tallon–Bosc, I.; Tasso, D.; Vakili, F.; Lühe, O. von der; Valtier, J. C.; Vannier, M.; Ventura, N.

doi:10.1051/0004-6361:20065719

Cited by 57 publications

(61 citation statements)

References 20 publications

(40 reference statements)

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“…AMBER/VLTI observations show that most of the K band continuum flux arises from a ring of radius R = 0.5 au (Tatulli et al 2007), in agreement with the location of the dust sublimation radius in the circumbinary disc (Garcia et al 2013). …”

Section: Introductionsupporting

confidence: 63%

Precession and accretion in circumbinary discs: the case of HD 104237

Dunhill

Cuadra

Dougados

2015

Monthly Notices of the Royal Astronomical Society

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We present the results of smoothed particle hydrodynamics (SPH) simulations of the disc around the young, eccentric stellar binary HD 104237. We find that the binary clears out a large cavity in the disc, driving a significant eccentricity at the cavity edge. This then precesses around the binary at a rate of˙ = 0.48 • T −1 b , which for HD 104237 corresponds to a precession period of 40 years. We find that the accretion pattern into the cavity and onto the binary changes with this precession, resulting in a periodic accretion variability driven purely by the physical parameters of the binary and its orbit. For each star we find that this results in order of magnitude changes in the accretion rate. We also find that the accretion variability allows the primary to accrete gas at a higher rate than the secondary for approximately half of each precession period. Using a large number of 3-body integrations of test particles orbiting different binaries, we find good agreement between the precession rate of a test particle and our SPH disc precession. These rates also agree very well with the precession rates predicted by the analytic theory of Leung & Lee (2013), showing that their prescription can be accurately used to predict long-term accretion variability timescales for eccentric binaries accreting from a disc. We discuss the implications of our result, and suggest that this process provides a viable way of preserving unequal mass ratios in accreting eccentric binaries in both the stellar and supermassive black hole regimes.

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Section: Introductionsupporting

confidence: 63%

Precession and accretion in circumbinary discs: the case of HD 104237

Dunhill

Cuadra

Dougados

2015

Monthly Notices of the Royal Astronomical Society

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“…. Martin-Zaïdi et al (2008) found excited and hot H 2 gas from far-UV spectra, while Tatulli et al (2007) explain the origin of the Brγ emission by an inner disk wind, originating at about 0.5 AU from the star.…”

Section: Stars With Measurements Suggestivementioning

confidence: 95%

“…For many of our targets with a detected magnetic field, reports on the detection of excited, hot inner disk gas exist, which may be attributed to a gaseous accretion ring close to the star (see especially Tatulli et al 2007;Isella et al 2008).…”

Section: Hot Disk Gasmentioning

confidence: 99%

Searching for a link between the magnetic nature and other observed properties of Herbig Ae/Be stars and stars with debris disks

Hubrig

Stelzer

Schöller

et al. 2009

A&A

Self Cite

100

149

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Context. Recently, evidence for the presence of weak magnetic fields in Herbig Ae/Be stars has been found in several studies. Aims. We seek to expand the sample of intermediate-mass pre-main sequence stars with circular polarization data to measure their magnetic fields, and to determine whether magnetic field properties in these stars are correlated with mass-accretion rate, disk inclination, companions, silicates, PAHs, or show a correlation with age and X-ray emission as expected for the decay of a remnant dynamo. Methods. Spectropolarimetric observations of 21 Herbig Ae/Be stars and six debris disk stars have been obtained at the European Southern Observatory with FORS 1 mounted on the 8 m Kueyen telescope of the VLT. With the GRISM 600B in the wavelength range 3250-6215 Å we were able to cover all hydrogen Balmer lines from Hβ to the Balmer jump. In all observations a slit width of 0. 4 was used to obtain a spectral resolving power of R ≈ 2000. Results. Among the 21 Herbig Ae/Be stars studied, new detections of a magnetic field were achieved in six stars. For three Herbig Ae/Be stars, we confirm previous magnetic field detections. The largest longitudinal magnetic field, B z = −454 ± 42 G, was detected in the Herbig Ae/Be star HD 101412 using hydrogen lines. No field detection at a significance level of 3σ was achieved in stars with debris disks. Our study does not indicate any correlation of the strength of the longitudinal magnetic field with disk orientation, disk geometry, or the presence of a companion. We also do not see any simple dependence on the mass-accretion rate. However, it is likely that the range of observed field values qualitatively supports the expectations from magnetospheric accretion models giving support for dipole-like field geometries. Both the magnetic field strength and the X-ray emission show hints of a decline with age in the range of ∼2-14 Myr probed by our sample, supporting a dynamo mechanism that decays with age. However, our study of rotation does not show any obvious trend of the strength of the longitudinal magnetic field with rotation period. Furthermore, the stars seem to obey the universal power-law relation between magnetic flux and X-ray luminosity established for the Sun and main-sequence active dwarf stars.

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“…Interferometric observations of the Brγ line show that the emission originates in a region more compact than the continuum, but more extended than the magnetosphere; its most likely origin is a stellar or disk wind (Kraus et al 2008). Other sources exhibit similar signatures in Brγ, attributed to an equatorial atomic disk wind within a few au of the star (Malbet et al 2007;Tatulli et al 2007;Eisner et al 2010;Benisty et al 2010b;Weigelt et al 2011).…”

Section: Kinematic Structure and Size Of The Launch Regionmentioning

confidence: 97%

Relating jet structure to photometric variability: the Herbig Ae star HD 163296

Ellerbroek

Podio

Dougados

et al. 2014

A&A

131

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Herbig Ae/Be stars are intermediate-mass pre-main sequence stars surrounded by circumstellar dust disks. Some are observed to produce jets, whose appearance as a sequence of shock fronts (knots) suggests a past episodic outflow variability. This "jet fossil record" can be used to reconstruct the outflow history. We present the first optical to near-infrared (NIR) spectra of the jet from the Herbig Ae star HD 163296, obtained with VLT/X-shooter. We determine the physical conditions in the knots and also their kinematic "launch epochs". Knots are formed simultaneously on either side of the disk, with a regular interval of ∼16 yr. The velocity dispersion versus jet velocity and the energy input are comparable between both lobes. However, the mass-loss rate, velocity, and shock conditions are asymmetric. We findṀ jet /Ṁ acc ∼ 0.01−0.1, which is consistent with magneto-centrifugal jet launching models. No evidence of any dust is found in the high-velocity jet, suggesting a launch region within the sublimation radius (<0.5 au). The jet inclination measured from proper motions and radial velocities confirms that it is perpendicular to the disk. A tentative relation is found between the structure of the jet and the photometric variability of the central source. Episodes of NIR brightening were previously detected and attributed to a dusty disk wind. We report for the first time significant optical fadings lasting from a few days up to a year, coinciding with the NIR brightenings. These are very likely caused by dust lifted high above the disk plane, and this supports the disk wind scenario. The disk wind is launched at a larger radius than the high-velocity atomic jet, although their outflow variability may have a common origin. No significant relation between outflow and accretion variability could be established. Our findings confirm that this source undergoes periodic ejection events, which may be coupled with dust ejections above the disk plane.

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Constraining the wind launching region in Herbig Ae stars: AMBER/VLTI spectroscopy of HD 104237

Cited by 57 publications

References 20 publications

Precession and accretion in circumbinary discs: the case of HD 104237

Precession and accretion in circumbinary discs: the case of HD 104237

Searching for a link between the magnetic nature and other observed properties of Herbig Ae/Be stars and stars with debris disks

Relating jet structure to photometric variability: the Herbig Ae star HD 163296

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