The Mass Accretion Rates of Intermediate-Mass T Tauri Stars

By N. Calvet, J. Muzerolle, C. Briceño, Jesús Hernández, L. Hartmann, José Luis Saucedo, K. Gordon. 2004

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In Astronomy and Astrophysics

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PHOTOEVAPORATION OF CIRCUMSTELLAR DISKS BY FAR-ULTRAVIOLET, EXTREME-ULTRAVIOLET AND X-RAY RADIATION FROM THE CENTRAL STAR (2008, methodology): “Using archival IUE data (Valenti et al. 2003), we find that the median fractional UV excess luminosity for stars with low accretion rates (we use a procedure similar to Calvet et al. (2004)) is given by ∼log (LUV,excess/L∗) = −3.3; we use this value.”
UV Excess Measures of Accretion onto Young Very Low Mass Stars and Brown Dwarfs (2008, background): “Accretion rate versus mass Figure 14 shows Ṁ versus M for Taurus accretors with AV < 2.5 from Gullbring et al. (1998), Hartigan & Kenyon (2003), Calvet et al. (2004), Muzerolle et al. (2005), and from the low-resolution Keck I and HST spectra analyzed in this work8.”
Theory of Star Formation (2007, background): “A recent compilation of observations (White & Basri, 2003; Muzerolle et al., 2003; Calvet et al., 2004) shows an approximate dependence of the accretion rate on stellar mass Ṁdisk ∝ m2∗, although with considerable scatter (Muzerolle et al., 2005).”
A spectroscopic survey of Herbig Ae/Be stars with X-shooter – I. Stellar parameters and accretion rates (2015, background): “The accretion rates obtained are observed to increase with both temperature and luminosity; this trend is seen in the literature for CTTs and HAeBes alike.”
A Survey and Analysis of Spitzer Infrared Spectrograph Spectra of T Tauri Stars in Taurus (2006, background): “Classical T Tauri stars in Taurus have average mass accretion rates of 10 8M yr 1; accretion rates seem to increase with themass of the star and also decrease over time (Calvet et al. 2004; Muzerolle et al. 2005; Hartmann et al. 1998).”
ACCRETION RATES FOR T TAURI STARS USING NEARLY SIMULTANEOUS ULTRAVIOLET AND OPTICAL SPECTRA (2013, background): “Calvet et al. (2004) analyzed NUV spectra for a sample of intermediate mass T Tauri stars and found that luminosities of C II] λ2325 Å and Mg II λ2800 Å increased with Lacc.”
The Truncated Disk of CoKu Tau/4 (2004, methodology): “Using an extinction law with RV ∼ 3.6, as indicated by the recent study of Calvet et al. (2004), this would suggest AV ∼ 3.”
The Sun in Time: Activity and Environment (2007, background): “Muzerolle et al. (2003), Muzerolle et al. (2005), and Calvet et al. (2004) described a relation between Ṁ and the stellar mass M , approximately reading Ṁ ∝ M2.”
PROTOPLANETARY DISK STRUCTURES IN OPHIUCHUS (2009, methodology): “…calculations use the Ṁ∗ values in Table 6, which were derived directly from emission line fluxes (or U -band excesses) in the literature using the standard data−accretion luminosity conversions (Muzerolle et al. 1998; Calvet et al. 2004) to force consistency with our adopted stellar properties.”
Accretion onto Pre-Main-Sequence Stars (2016, methodology): “Direct measurements of accretion rates have been made for intermediate-mass and HAeBe stars (Calvet et al. 2004, Donehew & Brittain 2011, Mendigutia et al. 2011, Fairlamb et al. 2015) down to the substellar regime (e.g., Herczeg et al. 2009, Rigliaco et al. 2012, Zhou et al. 2014).”
Accretion in the ρ-Ophiuchi pre-main sequence stars (2006, methodology): “The relation between IR line luminosity and accretion luminosity, independently measured from the UV excess, was established by Muzerolle et al. (1998b) for TTS, and by Calvet et al. (2004) for intermediate mass objects.”
TIME EVOLUTION OF VISCOUS CIRCUMSTELLAR DISKS DUE TO PHOTOEVAPORATION BY FAR-ULTRAVIOLET, EXTREME-ULTRAVIOLET, AND X-RAY RADIATION FROM THE CENTRAL STAR (2009, background): “This scaling is motivated by observations of a correlation between the accretion rate and central star mass, Ṁacc ∝ M2∗ (Muzerolle et al 2003, Natta et al 2004, Calvet et al. 2004, Muzerolle et al 2005, Natta et al 2006).”
Herbig Ae/Be Stars in nearby OB Associations (2004, background): “Calvet et al. (2004b) extended the correlation between mass accretion rate (Ṁ ) and stellar mass (M*) from Muzerolle et al. (2003a) to the intermediate-mass stars, up to 3.5 M ; in particular, they found that Ṁ / M 2 .”
Accretion Rates in Herbig Ae stars (2006, methodology): “Calvet et al. (2004) have shown that the correlation between the hydrogen IR line luminosity and the accretion luminosity found in TTS and BDs (Muzerolle et al. 1998; Natta et al. 2004) extends to their sample of IMTTS (see also van den Ancker 2004).”
A Spitzer Space Telescope Study of Disks in the Young σ Orionis Cluster (2007, background): “…indicated that the timescale for this evolution in disk emission is strongly dependent on the stellar mass (Lada&Lada 1995;Muzerolle et al. 2003;Calvet et al. 2004; Sicilia-Aguilar et al. 2005), ranging from 5 to 7 Myr for objects in the mass range of the T Tauri stars (TTSs; with spectral…”