The Mass Accretion Rates of Intermediate-Mass T Tauri Stars

Calvet, Nuria; Muzerolle, James; Briceño, César; Hernández, Jesús; Hartmann, L.; Saucedo, José Luis; Gordon, K. D.

doi:10.1086/422733

Cited by 403 publications

(613 citation statements)

References 81 publications

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“…This is near the bottom of the range of accretion rates observed for protoplanetary discs (Calvet et al 2004) and might be expected to occur during their late stages which are the focus of attention here. However, we have also considered disc models with surface density scaled such that they are up to ten times more massive and accordingly with a steady state accretion rate that is also up to ten times higher.…”

Section: Disc Model and Viscosity Prescriptionmentioning

confidence: 81%

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On the orbital evolution of a pair of giant planets in mean motion resonance

André

Papaloizou

2016

Mon. Not. R. Astron. Soc.

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Pairs of extrasolar giant planets in a mean motion commensurability are common with 2:1 resonance occurring most frequently. Disc-planet interaction provides a mechanism for their origin. However, the time scale on which this could operate in particular cases is unclear. We perform 2D and 3D numerical simulations of pairs of giant planets in a protoplanetary disc as they form and maintain a mean motion commensurability. We consider systems with current parameters similar to those of HD 155358, 24 Sextantis and HD 60532, and disc models of varying mass, decreasing mass corresponding to increasing age. For the lowest mass discs, systems with planets in the Jovian mass range migrate inwards maintaining a 2:1 commensurability. Systems with the inner planet currently at around 1 au from the central star could have originated at a few au and migrated inwards on a time scale comparable to protoplanetary disc lifetimes. Systems of larger mass planets such as HD 60532 attain 3:1 resonance as observed. For a given mass accretion rate, results are insensitive to the disc model for the range of viscosity prescriptions adopted, there being good agreement between 2D and 3D simulations. However, in a higher mass disc a pair of Jovian mass planets passes through 2:1 resonance before attaining a temporary phase lasting a few thousand orbits in an unstable 5:3 resonance prior to undergoing a scattering. Thus finding systems in this commensurability is unlikely.

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Section: Disc Model and Viscosity Prescriptionmentioning

confidence: 81%

“…In this way the disc-planet interaction at different stages of the life of the protoplanetary disc can be studied with lower mass discs corresponding to later stages (e.g. Calvet et al 2004).…”

Section: Introductionmentioning

confidence: 99%

On the orbital evolution of a pair of giant planets in mean motion resonance

André

Papaloizou

2016

Mon. Not. R. Astron. Soc.

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“…Correlations for other lines are available in the on-line version of this paper. The line luminosity-accretion luminosity relationship can be approximated by a power law, and has been in numerous works on CTTs and HAeBes (Muzerolle, Hartmann & Calvet 1998;Calvet et al 2004;Dahm 2008;Herczeg & Hillenbrand 2008;Mendigutía et al 2011;Rigliaco et al 2012), where :…”

Section: Accretion Luminosity -Line Luminosity Relationshipsmentioning

confidence: 99%

A spectroscopic survey of Herbig Ae/Be stars with X-Shooter – II. Accretion diagnostic lines

Fairlamb

Oudmaijer

Mendigutía

et al. 2016

Mon. Not. R. Astron. Soc.

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The Herbig Ae/Be stars (HAeBes) allow an exploration of the properties of PreMain Sequence(PMS) stars above the low-mass range (< 2 M ⊙ ) and those bordering the high-mass range (> 8 M ⊙ ). This paper is the second in a series exploring accretion in 91 HAeBes with Very Large Telescope/X-shooter spectra. Equivalent width measurements are carried out on 32 different lines, spanning the UV to NIR, in order to obtain their line luminosities. The line luminosities were compared to accretion luminosities, which were determined directly from measurements of an UV-excess. When detected, emission lines always demonstrate a correlation with the accretion luminosity, regardless of detection frequency. The average relationship between accretion luminosity and line luminosity is found to be L acc ∝ L line 1.16±0.15 . This is in agreement with the findings in Classical T Tauri stars, although the HAeBe relationship is generally steeper, particularly towards the Herbig Be mass range. Since all observed lines display a correlation with the accretion luminosity, all of them can be used as accretion tracers. This has increased the number of accretion diagnostic lines in HAeBes tenfold. However, questions still remain on the physical origin of each line, which may not be due to accretion.

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“…In x 2 of the paper we describe our sample. Spectroscopic observations obtained are presented in Baines et al 2004;(18) Malfait et al 1998;(19) Acke et al 2005;(20) Testi et al 1998;(21) van den Ancker et al 2004;(22) Corcoran & Ray 1998;(23) Miroshnichenko et al 2001b;(24) Alencar et al 2003;(25) Hamaguchi et al 2005;(26) Terranegra et al 1994;(27) van den Ancker et al 1998;(28) Berrilli et al 1992;(29) Perryman et al 1997;(30) Calvet et al 2004;(31) Leinert et al 1997;(32) Kawamura et al 1998;(33) Hernández et al 2005;(34) Herbst & Racine 1976;(35) Herbst et al 1982;(36) Shevchenko et al 1999;(37) Leinert et al 2004;(38) Eisner et al 2004;(39) Shevchenko & Yakubov 1989. x 3. Main results of our study are presented in x 4 and discussed in detail in x 5.…”

Section: Introductionmentioning

confidence: 99%

Evolution of Emission‐Line Activity in Intermediate‐Mass Young Stars

Manoj

Bhatt

Maheswar

et al. 2006

ApJ

140

139

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We present optical spectra of 45 intermediate-mass Herbig Ae/ Be stars. Together with the multiepoch spectroscopic and photometric data compiled for a large sample of these stars and ages estimated for individual stars by using preYmain-sequence evolutionary tracks, we have studied the evolution of emission-line activity in them. We find that, on average, the H emission line strength decreases with increasing stellar age in Herbig Ae/ Be stars, indicating that the accretion activity gradually declines during the preYmain-sequence phase. This would hint at a relatively longlived (a few Myr) process being responsible for the cessation of accretion in Herbig Ae/ Be stars. We also find that the accretion activity in these stars drops substantially by $3 Myr. This is comparable to the timescale in which most intermediate-mass stars are thought to lose their inner disks, suggesting that inner disks in intermediate-mass stars are dissipated rapidly after the accretion activity has fallen below a certain level. We further find a relatively tight correlation between strength of the emission line and near-infrared excess due to inner disks in Herbig Ae/ Be stars, indicating that the disks around Herbig Ae/ Be stars cannot be entirely passive. We suggest that this correlation can be understood within the framework of the puffed-up inner rim disk models if the radiation from the accretion shock is also responsible for the disk heating.

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The Mass Accretion Rates of Intermediate-Mass T Tauri Stars

Cited by 403 publications

References 81 publications

On the orbital evolution of a pair of giant planets in mean motion resonance

On the orbital evolution of a pair of giant planets in mean motion resonance

A spectroscopic survey of Herbig Ae/Be stars with X-Shooter – II. Accretion diagnostic lines

Evolution of Emission‐Line Activity in Intermediate‐Mass Young Stars

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