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Mid-infrared Variability and Accretion in NGC 2264 Protostars

Published online by Cambridge University Press:  27 January 2016

S. Terebey ,
A. M. Cody ,
L. M. Rebull  and
J. R. Stauffer
S. Terebey
Affiliation:
California State University Los Angeles; email: sterebe@calstatela.edu
A. M. Cody
Affiliation:
NASA Ames Research Center;
L. M. Rebull
Affiliation:
Spitzer Science Center; California Institute of Technology
J. R. Stauffer
Affiliation:
Spitzer Science Center; California Institute of Technology
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Abstract

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Variable mass accretion is thought to be an important aspect of protostar formation. Mid-infrared wavelength observations trace variations in accretion luminosity and thus can probe mass accretion on sub-AU scales. We present results from the Spitzer YSOVAR campaign towards Class I protostars in NGC 2264. The precise (0.02 mag) medium-cadence light curves at 3.6 and 4.5 microns show that young star variability is ubiquitous, with a variety of morphologies and time scales. A structure function analysis shows the light curves, on average, have a power-law behavior up to 30 days. The trend continues to longer timescales (years) for protostars (Class I), in contrast with the smaller brightness changes displayed by T Tauri stars (Class II). The power-law behavior suggests a stochastic process, such as turbulent mass accretion, drives the variability.

Keywords

stars:formation – stars:protostars – stars:variables: T Tauri
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 10 , Issue S314: Young Stars & Planets Near the Sun , November 2015 , pp. 209 - 210
Copyright
Copyright © International Astronomical Union 2016 

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