Accretion in the ρ-Ophiuchi pre-main sequence stars

By A. Natta, L. Testi, S. Randich. 2006

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Aims. The aim of this paper is to provide a measurement of the mass accretion rate in a large, complete sample of objects in the core of the star forming region p Oph. Methods. The sample includes most of the objects (104 out of 111) with evidence of a circumstellar disk from mid-infrared photometry; it covers a stellar mass range from about 0.03 to 3 M ⊙ and it is complete to a limiting mass of ∼0.05 M ⊙ . We used J and K-band spectra to derive the mass accretion rate of each object from the intensity of the hydrogen recombination lines, Pap or Bry. For comparison, we also obtained similar spectra of 35 diskless objects. Results. The results show that emission in these lines is only seen in stars with disks, and can be used as an indicator of accretion. However, the converse does not hold, as about 50% of our disk objects do not have detectable line emission. The measured accretion rates show a strong correlation with the mass of the central object (Mace oc M 1.8±0.2 *) and a large spread, of two orders of magnitude at least, for any interval of M*. A comparison with existing data for Taurus shows that the objects in the two regions have similar behaviour, at least for objects more massive than ∼0.1 M ⊙ . The implications of these results are briefly discussed.

Subfields: Astronomy and Astrophysics, Spectroscopy

View Paper: https://www.semanticscholar.org/paper/936540daa3899e994acc007db3a791c6422d39e3

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Citations in the corpus

Accretion-driven turbulence as universal process: galaxies, molecular clouds, and protostellar disks (2009, methodology): “where α ≈ 1.8, however, with a large scatter of about one order of magnitude (Muzerolle et al. 2003; Natta et al. 2006).”
X-Shooter study of accretion in Chamaeleon I (2015, methodology): “Relations between the accretion luminosity (Lacc) and stellar luminosity (L?, e.g., Natta et al. 2006; Clarke & Pringle 2006; Rigliaco et al. 2011a; Manara et al. 2012) and between Ṁacc and stellar mass (M?, e.g., Muzerolle et al. 2003; Mohanty et al. 2005; Natta et al. 2006; Herczeg & Hillenbrand…”
ALMA continuum observations of the protoplanetary disk AS 209. Evidence of multiple gaps opened by a single planet (2017, background): “= 1.5 L , Tazzari et al. 2016) is part of the young (age ∼ 0.5–1.0 Myr; Natta et al. 2006) Ophiuchus star forming region at a distance of 126 pc from the Sun (Gaia Collaboration 2016).”
PROTOPLANETARY DISK STRUCTURES IN OPHIUCHUS (2009, background): “Despite these substantial disk signatures, the standard hallmarks of accretion for the DoAr 25 disk are comparatively meager: estimates of the mass accretion rate range from low (3 × 10−9 M⊙ yr−1; Greene & Lada 1996; Luhman & Rieke 1999) to negligible (< 2 × 10−10 M⊙ yr−1; Natta et al. 2006) values.”
Radiation-hydrodynamic models of X-ray and EUV photoevaporating protoplanetary discs (2009, result): “The wind mass loss rate is now comparable with typical accretion rates measured in Classical T Tauri stars (Natta et al. 2006).”
High-Resolution Submillimeter Constraints on Circumstellar Disk Structure (2006, background): “Although it may be more likely that the IRAS photometry for this source is contaminated by extended cloud emission, we can also not rule out a central hole similar toGMAur, especially given the limit placed on themass accretion rate, Ṁ P 6 ; 10 10 M yr 1 (Natta et al. 2006).”
A Decreased Probability of Habitable Planet Formation around Low-Mass Stars (2007, background): “Additional clues come from the observed stellar accretion rate Ṁ , which scales as Ṁ ∝ M2⋆ , with a large dispersion (Muzerolle et al. 2003, 2005, Natta et al. 2006).”
A STEEPER THAN LINEAR DISK MASS–STELLAR MASS SCALING RELATION (2016, background): “…was corroborated by the observation that stellar accretion rates (Ṁ ), tracing the gas disk component, display a steeper dependence with stellar mass when the population of lowmass stars is well sampled (e.g., Natta et al. 2006; Fang et al. 2009; Rigliaco et al. 2011; Alcalá et al. 2014).”
Star and Protoplanetary Disk Properties in Orion's Suburbs (2009, background): “Power law fits of the formṀacc∝Mα∗ have yielded values in the range 1.0−2.1 for the exponentα (White & Basri 2003; Muzerolle et al. 2003; Calvet et al. 2004; Muzerolle et al. 2005; Mohanty et al. 2005; Natta et al. 2006; Garcia Lopez et al. 2006; Herczeg & Hillenbrand 2008; Gatti et al. 2008).”
UV Excess Measures of Accretion onto Young Very Low Mass Stars and Brown Dwarfs (2008, background): “These diagnostics are often more accessible than modelling Hα profiles or measuring the UV excess and are particularly useful for variability studies of a individual objects (e.g. Alencar et al. 2005; Azevedo et al. 2006) or in large samples (Natta et al. 2006).”
Accretion disks in luminous young stellar objects (2015, background): “Natta et al. (2006) estimate Ṁacc for a sample of T Tauri stars in the ρ-Ophiuchi starforming region from Brγ line emission.”
Accretion Rates in Herbig Ae stars (2006, methodology): “2 compares thėMacc distribution of the HAe stars to that of objects in Ophiuchus in two mass ranges, as labelled.”
Characterizing Young Brown Dwarfs Using Low-Resolution Near-Infrared Spectra (2006, background): “Mass accretion rates (based on H emission) depend strongly on the mass of the central source, with Ṁ / M 2 for masses from 150MJ down to roughly 25MJ (Muzerolle et al. 2005; Natta et al. 2006).”
Dust grain growth in ρ-Ophiuchi protoplanetary disks (2010, methodology): “7 For IRS 41, for which the 2MASS J-band flux is not available, we adopted the luminosities as derived by Natta et al. (2006), after correcting them by a multiplicative factor (130 pc/150 pc)2 to account for the different adopted distance of 150 pc in the Natta et al. paper.”