Exploring the circumstellar environment of the young eruptive star V2492 Cygni
Exploring the circumstellar environment of the young eruptive star V2492 Cygni
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DOI：
10.1051/0004-6361/201220553
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发表时间：
2013-01
影响因子：
6.5
通讯作者：
Á. Kóspál;P. Ábrahám;J. Acosta-Pulido;J. Acosta-Pulido;M. Morales;M. Morales;Z. Balog;M. I. Carnerero;M. I. Carnerero;E. Szegedi-Elek;A. Farkas;T. Henning;J. Kelemen;Tamas G. Kovacs;Mária Kun;G'abor Marton;Sz. Mészáros;Sz. Mészáros;A. Moór;A. Pál;A. Pál;K. Sárneczky;K. Sárneczky;R. Szakáts;N. Szalai;A. Szing;Imre Péter Tóth;N. J. Turner;K. Vida
中科院分区：
文献类型：
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作者：
Á. Kóspál;P. Ábrahám;J. Acosta-Pulido;J. Acosta-Pulido;M. Morales;M. Morales;Z. Balog;M. I. Carnerero;M. I. Carnerero;E. Szegedi-Elek;A. Farkas;T. Henning;J. Kelemen;Tamas G. Kovacs;Mária Kun;G'abor Marton;Sz. Mészáros;Sz. Mészáros;A. Moór;A. Pál;A. Pál;K. Sárneczky;K. Sárneczky;R. Szakáts;N. Szalai;A. Szing;Imre Péter Tóth;N. J. Turner;K. Vida
上下文天鹅座V2492是一颗年轻的爆发型星星，于2010年爆发。自爆发峰以来观察到的近红外颜色变化表明，该源属于一个新定义的年轻爆发恒星子类，其中随时间变化的吸积和可变的视线消光在流量变化中起着综合作用。目标。为了了解光变化的起源，并探索V2492 Cyg的星周和星际环境，我们在10个不同的波长下监测了该光源，从地面到2.2 μm之间，从空间到3.6 μm到160 μm之间。方法.我们分析了光变曲线，并通过与标准红化路径的比较研究了色-色图。我们通过计算远红外数据的温度和光学深度图来研究V2492 Cyg的分子云结构。结果我们发现，在不同波长的光变曲线的形状是严格自相似的，所观察到的变化是一个单一的物理过程，最有可能的变量消光。我们认为，中央源是由一个密集的尘埃云在内部磁盘的episodically掩盖，根据远红外通量的不变性，我们建议，这是一个长期的，而不是一个短暂的结构。在某些方面，天鹅座V2492可以被认为是一颗年轻的猎户座UX型恒星。结论.天鹅座V2492的例子表明，年轻爆发恒星的光变化并不完全与吸积变化有关。的变化提供了信息的一个方位角不对称的结构元素的内盘。地球带的这种不对称密度分布也可能对行星形成的初始条件产生影响。
Context. V2492 Cyg is a young eruptive star that went into outburst in 2010. The near-infrared color changes observed since the outburst peak suggest that the source belongs to a newly defined sub-class of young eruptive stars, where time-dependent accretion and variable line-of-sight extinction play a combined role in the flux changes. Aims. In order to learn about the origin of the light variations and to explore the circumstellar and interstellar environment of V2492 Cyg, we monitored the source at ten different wavelengths, between 0.55 μm and 2.2 μm from the ground and between 3.6 μm and 160 μm from space. Methods. We analyze the light curves and study the color−color diagrams via comparison with the standard reddening path. We examine the structure of the molecular cloud hosting V2492 Cyg by computing temperature and optical depth maps from the far-infrared data. Results. We find that the shapes of the light curves at different wavelengths are strictly self-similar and that the observed variability is related to a single physical process, most likely variable extinction. We suggest that the central source is episodically occulted by a dense dust cloud in the inner disk and, based on the invariability of the far-infrared fluxes, we propose that it is a long-lived rather than a transient structure. In some respects, V2492 Cyg can be regarded as a young, embedded analog of UX Orionis-type stars. Conclusions. The example of V2492 Cyg demonstrates that the light variations of young eruptive stars are not exclusively related to changing accretion. The variability provided information on an azimuthally asymmetric structural element in the inner disk. Such an asymmetric density distribution in the terrestrial zone may also have consequences for the initial conditions of planet formation.