Abstract
Context. The accretion process has a central role in the formation of stars and planets.
Aims. We aim at characterizing the accretion properties of several hundred members of the star-forming cluster NGC2264 (3 Myr).
Methods. We performed a deep ugri mapping as well as a simultaneous u-band+r-band monitoring of the star-forming region with CFHT/MegaCam in order to directly probe the accretion process onto the star from UV excess measurements. Photometric properties and stellar parameters are determined homogeneously for about 750 monitored young objects, spanning the mass range ~0.1-2 M⊙. About 40% of the sample are classical (accreting) T Tauri stars, based on various diagnostics (Hα, UV and IR excesses). The remaining non-accreting members define the (photospheric + chromospheric)reference UV emission level over which flux excess is detected and measured.
Results. We revise the membership status of cluster members based on UV accretion signatures, and report a new population of50 classical T Tauri star (CTTS) candidates. A large range of UV excess is measured for the CTTS population, varying from a few times 0.1 to ~3mag. We convert these values to accretion luminosities and accretion rates, via a phenomenological description of the accretion shock emission. We thus obtain mass accretion rates ranging from a few10-10 to ~10-7 M⊙/yr. Taking into account a mass-dependent detection threshold for weakly accreting objects, we find a >6σ correlation between mass accretion rate and stellar mass. A power-law fit, properly accounting for censored data(upper limits), yields Ṁacc ∝ M*1.4±0.3. At any given stellar mass, we find a large spread of accretion rates, extending over about 2 orders of magnitude. The monitoring of the UV excess on a timescale of a couple of weeks indicates that its variability typically amounts to 0.5 dex, i.e., much smaller than the observed spread in accretion rates. We suggest that a non-negligible age spread across the star-forming region may effectively contribute to the observed spread in accretion rates at a given mass. In addition, different accretion mechanisms (like, e.g.,short-lived accretion bursts vs. more stable funnel-flow accretion) maybe associated to different Ṁacc regimes. Conclusions. A huge variety of accretion properties is observed for young stellar objects in the NGC 2264 cluster. While a definite correlation seems to hold between mass accretion rate and stellar mas sover the mass range probed here, the origin of the large intrinsic spread observed in mass accretion rates at any given mass remains to be explored.
Aims. We aim at characterizing the accretion properties of several hundred members of the star-forming cluster NGC2264 (3 Myr).
Methods. We performed a deep ugri mapping as well as a simultaneous u-band+r-band monitoring of the star-forming region with CFHT/MegaCam in order to directly probe the accretion process onto the star from UV excess measurements. Photometric properties and stellar parameters are determined homogeneously for about 750 monitored young objects, spanning the mass range ~0.1-2 M⊙. About 40% of the sample are classical (accreting) T Tauri stars, based on various diagnostics (Hα, UV and IR excesses). The remaining non-accreting members define the (photospheric + chromospheric)reference UV emission level over which flux excess is detected and measured.
Results. We revise the membership status of cluster members based on UV accretion signatures, and report a new population of50 classical T Tauri star (CTTS) candidates. A large range of UV excess is measured for the CTTS population, varying from a few times 0.1 to ~3mag. We convert these values to accretion luminosities and accretion rates, via a phenomenological description of the accretion shock emission. We thus obtain mass accretion rates ranging from a few10-10 to ~10-7 M⊙/yr. Taking into account a mass-dependent detection threshold for weakly accreting objects, we find a >6σ correlation between mass accretion rate and stellar mass. A power-law fit, properly accounting for censored data(upper limits), yields Ṁacc ∝ M*1.4±0.3. At any given stellar mass, we find a large spread of accretion rates, extending over about 2 orders of magnitude. The monitoring of the UV excess on a timescale of a couple of weeks indicates that its variability typically amounts to 0.5 dex, i.e., much smaller than the observed spread in accretion rates. We suggest that a non-negligible age spread across the star-forming region may effectively contribute to the observed spread in accretion rates at a given mass. In addition, different accretion mechanisms (like, e.g.,short-lived accretion bursts vs. more stable funnel-flow accretion) maybe associated to different Ṁacc regimes. Conclusions. A huge variety of accretion properties is observed for young stellar objects in the NGC 2264 cluster. While a definite correlation seems to hold between mass accretion rate and stellar mas sover the mass range probed here, the origin of the large intrinsic spread observed in mass accretion rates at any given mass remains to be explored.
| Original language | English |
|---|---|
| Article number | A82 |
| Number of pages | 68 |
| Journal | Astronomy & Astrophysics |
| Volume | 570 |
| DOIs | |
| Publication status | Published - 21 Oct 2014 |
Keywords
- Accretion
- Accretion disks
- Stars: formation
- Stars: low-mass
- Stars: pre-main sequence
- Ultraviolet: stars
- Open clusters and associations: individual: NGC 2264