ON THE MID-INFRARED VARIABILITY OF CANDIDATE ERUPTIVE VARIABLES (EXORS): A COMPARISON BETWEEN SPITZER AND WISE DATA
ON THE MID-INFRARED VARIABILITY OF CANDIDATE ERUPTIVE VARIABLES (EXORS): A COMPARISON BETWEEN SPITZER AND WISE DATA
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关于候选爆发变量（EXORS）的中红外变率：斯皮策和怀斯数据之间的比较
DOI：
10.1088/0004-637x/782/1/51
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发表时间：
2014
期刊：
影响因子：
--
通讯作者：
D. Lorenzetti
中科院分区：
文献类型：
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作者：
S. Antoniucci;T. Giannini;G. Causi;D. Lorenzetti
为了统计研究年轻恒星物体中红外的变化性，我们将属于 C2D（核心到盘）遗留计划的 1478 个源的 3.6、4.5 和 24μm 斯皮策通量与 WISE 的 3.4、4.6 和 22μm 通量进行了比较。通过比较，我们选择了 34 个可变源的稳健样本。它们的变化按照光谱类别（根据广泛接受的 I 类/扁平/II/III 类原恒星方案）和每个恒星形成区域进行分类。平均而言，变量源的数量随着等级的增加而减少，并且英仙座和蛇夫座的变量源数量肯定高于变色龙和天狼星。根据类=进化范式，光度变异性可以被认为是进化程度较低的原恒星中更明显的特征，因此与吸积过程相关。此外，我们的统计结果与当前对不同区域恒星形成活动的认识一致。进一步研究了 34 个选定的变量与已知的年轻喷发变量（即 EXors）的相似性。特别是，我们分析了（1）光谱能量分布的形状，（2）恒星光球层的红外过剩，（3）星等与颜色变化，以及（4）模型拟合的输出参数。对 EXor 的首次系统搜索最终找到了 11 名真正的候选人，可以将其视为监控或未来调查的合适目标。
Aiming to statistically study the variability in the mid-IR of young stellar objects, we have compared the 3.6, 4.5, and 24 μm Spitzer fluxes of 1478 sources belonging to the C2D (Cores to Disks) legacy program with the WISE fluxes at 3.4, 4.6, and 22 μm. From this comparison, we have selected a robust sample of 34 variable sources. Their variations were classified per spectral Class (according to the widely accepted scheme of Class I/flat/II/III protostars), and per star forming region. On average, the number of variable sources decreases with increasing Class and is definitely higher in Perseus and Ophiuchus than in Chamaeleon and Lupus. According to the paradigm Class ≡ Evolution, the photometric variability can be considered to be a feature more pronounced in less evolved protostars, and, as such, related to accretion processes. Moreover, our statistical findings agree with the current knowledge of star formation activity in different regions. The 34 selected variables were further investigated for similarities with known young eruptive variables, namely the EXors. In particular, we analyzed (1) the shape of the spectral energy distribution, (2) the IR excess over the stellar photosphere, (3) magnitude versus color variations, and (4) output parameters of model fitting. This first systematic search for EXors ends up with 11 bona fide candidates that can be considered as suitable targets for monitoring or future investigations.