Emission-Line Diagnostics of T Tauri Magnetospheric Accretion. II. Improved Model Tests and Insights into Accretion Physics

By J. Muzerolle, N. Calvet, L. Hartmann. 2001

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In Astronomy and Astrophysics

Citations in the corpus

Star and Protoplanetary Disk Properties in Orion's Suburbs (2009, background): “…the central star can be estimated from the infrared excess, veiling in optical spectra, and emission lines that are thought to be due to magnetospheric accretion (Hillenbrand et al. 1992; Hartigan et al.1995; Gullbring et al. 1998; Muzerolle et al. 1998b; Calvet et al. 2000; Muzerolle et al. 2001).”
Measuring Accretion in Young Substellar Objects: Approaching the Planetary Mass Regime (2005, background): “…1995; Valenti et al. 1993; Gullbring et al. 1998; Calvet &Gullbring 1998), broad permitted emission lines produced in the ballistic magnetospheric gas flows (Muzerolle et al. 2001, hereafter MCH01), and forbidden emission lines produced in accretion-powered winds and jets (Hartigan et al. 1995).”
On the formation of Hα line emission around classical T Tauri stars (2006, methodology): “Muzerolle et al. (2001) also pointed out that the observed Hα profiles from CTTS typically have the wings extending to 500 km s−1(e.g. Edwards et al. 1994; Reipurth et al. 1996) which cannot be explained by the infall velocity alone.”
Probing T Tauri Accretion and Outflow with 1 Micron Spectroscopy (2006, background): “…and broad emission sometimes accompanied by redshifted absorption below the continuum and/or narrow centered emission, are attributed to formation in magnetospheric funnel flows and accretion shocks on the stellar surface (Edwards et al. 1994; Muzerolle et al. 2001; Herczeg et al. 2002, 2005).”
PHOTOEVAPORATION OF CIRCUMSTELLAR DISKS BY FAR-ULTRAVIOLET, EXTREME-ULTRAVIOLET AND X-RAY RADIATION FROM THE CENTRAL STAR (2008, background): “Considerable amounts of high-energy radiation from the star are initially absorbed at the base of the accretion column and in the wind (e.g., Muzerolle et al. 2001).”
Accretion dynamics and disk evolution in NGC 2264: a study based on the Corot photometric observations (2010, methodology): “…⋆ The CoRoT space mission was developed and is operated by the French space agency CNES, with participation of ESA’s RSSD and Science Programmes, Austria, Belgium, Brazil, Germany, and Spain (Shu et al., 1994; Hartmann et al., 1994; Muzerolle et al., 2001; Kurosawa et al., 2006).”
Three-dimensional Simulations of Disk Accretion to an Inclined Dipole. II. Hot Spots and Variability (2004, background): “This may possibly explain the observed variation of the shapes of magnetospheric lines with the accretion rate (Muzerolle et al. 2001).”
The Magnetic Fields of Classical T Tauri Stars (2007, background): “Muzerolle et al. (2001) note that current theory predicts a correlation between rotation period andmass accretion rate, which they do not observe.”
Accretion in brown dwarfs: An infrared view (2004, background): “The comparison of the observed profiles with those predicted by magnetospheric accretion models (Muzerolle et al. 2001) shows that five objects are actively accreting, with Ṁac in the range ∼ 10−9 − 10−11 M⊙/yr, while the remaining three in Cha I have narrow and symmetric profiles, and Ṁac<∼10…”
UV Excess Measures of Accretion onto Young Very Low Mass Stars and Brown Dwarfs (2008, methodology): “…in opticallythick post-shock gas, the Balmer continuum emission is produced in optically-thin pre-shock gas, and the Balmer line emission is mostly produced primarily in the magnetospheric accretion column (Hartmann et al. 1994; Calvet & Gullbring 1998; Muzerolle et al. 2001; Kurosawa et al. 2006).”
The T Tauri Phase Down to Nearly Planetary Masses: Echelle Spectra of 82 Very Low Mass Stars and Brown Dwarfs (2005, background): “…evincing broad line wings extending out to a few hundred kilometers per second from line center; the broadening is due to both the high (free-fall) velocity of the ac- creting gas and the large damping wings associated with Stark broadening in this very optically thick line (Muzerolle et al. 2001).”
Optical Spectroscopy of the Surface Population of the ρ Ophiuchi Molecular Cloud: The First Wave of Star Formation (2005, background): “…shape of the emission proﬁle also appeared to change in three cases (Chini 8, EL 24, and These broad H (cid:2) proﬁles, which can exceed 300 km s (cid:1) 1 in our sample, have been successfully modeled as arising in magneto-spheric accretion columns (Hartmann et al. 1994; Muzerolle et al. 2001).”
Accretion onto Pre-Main-Sequence Stars (2016, background): “…along axisymmetric, dipolar magnetic field lines have been successful in explaining line profiles of Balmer lines in CTTS (Hartmann et al. 1994; Muzerolle et al. 1998, 2001), in brown dwarfs (Muzerolle et al. 2000, 2003), and in some Herbig Ae (HAe) stars www.annualreviews.org • Accretion onto…”
Magnetospheres and Disk Accretion in Herbig Ae/Be Stars (2004, methodology): “We begin by analyzing a specific object of special interest, UX Ori, in terms of a magnetospheric accretion model similar to that developed by Muzerolle et al. (1998, 2001).”
Accretion in Young Stellar/Substellar Objects (2003, methodology): “Consistent with previous results on the evolution of disk accretion in higher mass, 0.5 M , stars (see, e.g., Muzerolle et al. 2000b, 2001b), we find here an accretion timescale on the order of several Myr for objects near the substellar boundary.”