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首页> 外文期刊>Astronomy and astrophysics >REM near-IR and optical photometric monitoring of pre-main sequence stars in Orion - Rotation periods and starspot parameters
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REM near-IR and optical photometric monitoring of pre-main sequence stars in Orion - Rotation periods and starspot parameters

机译：猎户座主前序列恒星的REM近红外和光学光度监测-旋转周期和星点参数

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Aims. We aim at determining the rotational periods and thestarspot properties in very young low-mass stars belonging to the OriOB1c star forming region, contributing to the study of the angularmomentum and magnetic activity evolution in these objects. Methods. We performed an intensive photometric monitoring of the PMS stars falling in a field of about 10in the vicinity of the Orion nebula cluster (ONC), also containing theBD eclipsing system 2MASSJ05352184-0546085. Photometric data werecollected between November 2006 and January 2007 with the REM telescopein the bands. The largest number of observations is in the Iband (about 2700images) and inJ and Hbands(about 500images in each filter). From the observed rotationalmodulation, induced by the presence of surface inhomogeneities, wederived the rotation periods. The long time-baseline (nearly threemonths) allowed us to detect rotation periods, also for the slowestrotators, with sufficient accuracy ().The analysis of the spectral energy distributions and, for some stars,of high-resolution spectra provided us with the main stellar parameters(luminosity, effective temperature, mass, age, and )which are essential for the discussion of our results. Moreover, thesimultaneous observations in six bands, spanning from optical tonear-infrared wavelengths, enabled us to derive the starspot propertiesfor these very young low-mass stars. Results. In total, we were able to determine the rotationperiods for 29stars, spanning from about0.6 to20days. Thanks to the relatively long time-baseline of ourphotometry, we derived periods for 16stars and improved previousdeterminations for the other13. We also report the serendipitousdetection of two strong flares in two of these objects. In most cases,the light-curve amplitudes decrease progressively from theR to Hbandas expected for cool starspots, while in a few cases, they can only bemodelled by the presence of hot spots, presumably ascribable tomagnetospheric accretion. The application of our own spot model to thesimultaneous light curves in different bands allowed us to deduce thespot parameters and particularly to disentangle the spot temperatureand size effects on the observed light curves. Key words: stars: pre-main sequence - stars: rotation - stars: starspots - stars: flare - techniques: photometric - ISM: individual objects: Orion
机译：目的我们旨在确定属于OriOB1c恒星形成区域的非常年轻的低质量恒星的自转周期和星点特性，从而有助于研究这些物体的角动量和磁活动演变。方法。我们对Orion星云团（ONC）附近大约10个场中坠落的PMS恒星进行了密集的光度监测，该恒星还包含BD蚀食系统2MASSJ05352184-0546085。光度数据是在2006年11月至2007年1月之间使用REM望远镜收集的。观察次数最多的是Iband（约2700个图像），inJ和Hband（每个滤镜中约500个图像）。从观察到的由表面不均匀性的存在引起的旋转调制，得出旋转周期。较长的时间基准（将近三个月）使我们能够以足够的精度（）检测最慢的旋转器的自转周期。对光谱能量分布以及某些恒星的高分辨率光谱的分析为我们提供了主要的恒星参数（发光度，有效温度，质量，年龄和）对于讨论我们的结果至关重要。此外，从光学声调红外波长开始的六个波段的同时观测，使我们能够推导这些非常年轻的低质量恒星的星点特性。结果。总的来说，我们能够确定29颗星的轮换周期，大约从0.6天到20天不等。由于光度法的时间基准相对较长，我们得出了16个星的周期，并改进了其他16个星的先前确定性。我们还报告了在其中两个物体中两个强光弹的意外发现。在大多数情况下，光曲线的振幅从凉爽的星点预期的R逐渐降低到Hbandas，而在少数情况下，只能由热点的存在来建模，大概是由于磁层的积聚。通过将我们自己的光斑模型应用于不同波段的同时光曲线，我们可以推导出光斑参数，尤其是可以解开光斑温度和大小对观察到的光曲线的影响。关键词：恒星：主序前-恒星：自转-恒星：星点-恒星：耀斑-技术：光度学-ISM：单个物体：猎户座

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