Milliarcsecond N-Band Observations of the Nova RS Ophiuchi: First Science with the Keck Interferometer Nuller
Milliarcsecond N-Band Observations of the Nova RS Ophiuchi: First Science with the Keck Interferometer Nuller
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DOI：
10.1086/529422
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发表时间：
2008-01
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通讯作者：
R. Barry;R. Barry;W. Danchi;W. Traub;J. Sokoloski;J. Wisniewski;E. Serabyn;M. Kuchner;R. Akeson;E. Appleby;J. Bell;A. Booth;H. Brandenburg;M. Colavita;S. Crawford;M. Creech-Eakman;W. Dahl;C. Felizardo;Javier A. García;J. Gathright;M. Greenhouse;J. Herstein;E. Hovland;M. Hrynevych;C. Koresko;R. Ligon;B. Mennesson;R. Millan-Gabet;D. Morrison;D. Palmer;T. Panteleeva;S. Ragland;M. Shao;R. Smythe;K. Summers;M. Swain;K. Tsubota;C. Tyau;E. Wetherell;P. Wizinowich;J. Woillez;G. Vasisht
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作者：
R. Barry;R. Barry;W. Danchi;W. Traub;J. Sokoloski;J. Wisniewski;E. Serabyn;M. Kuchner;R. Akeson;E. Appleby;J. Bell;A. Booth;H. Brandenburg;M. Colavita;S. Crawford;M. Creech-Eakman;W. Dahl;C. Felizardo;Javier A. García;J. Gathright;M. Greenhouse;J. Herstein;E. Hovland;M. Hrynevych;C. Koresko;R. Ligon;B. Mennesson;R. Millan-Gabet;D. Morrison;D. Palmer;T. Panteleeva;S. Ragland;M. Shao;R. Smythe;K. Summers;M. Swain;K. Tsubota;C. Tyau;E. Wetherell;P. Wizinowich;J. Woillez;G. Vasisht
我们报告了新星蛇夫座RS （RS Oph）使用凯克干涉仪Nuller （KIN）的观测，大约在2006年2月12日爆发后的3.8天。这些观测结果代表了KIN在8到12.5 μm的N波段以零化模式工作的第一个科学结果。零化技术是一种稀疏孔径技术，相当于填充口径望远镜中使用的传统日冕技术。在这种模式下，恒星本身的光被破坏性条纹所抑制，有效地增强了恒星附近星周物质的对比度。通过拟合独特的KIN数据，我们获得了圆盘型、高斯型和壳型中红外连续发射材料的角尺寸分别为6.2、4.0和5.4 mas。数据显示，相对于白矮星（WD）的外部区域，位于白矮星（WD）附近的内部空间区域的中性原子氢和原子金属（包括硅）的发射增强。此外，星云发射线和热硅酸盐尘埃的证据也存在于外层空间区域，中心位于距WD约17 AU处，而这在内部区域是没有发现的。我们的证据表明，在爆炸波到达这些区域之前，这些特征已经被外层空间的新星闪光所激发。这些鉴定支持一个模型，其中尘埃似乎存在于爆发之间，而不是在爆发事件期间产生的。我们进一步根据系统的统一模型来讨论目前的结果，该模型包括两颗恒星轨道平面上密度的增加，这是由恒星通过红巨星的冷风运动引起的螺旋激波造成的。
We report observations of the nova RS Ophiuchi (RS Oph) using the Keck Interferometer Nuller (KIN), approximately 3.8 days following the most recent outburst that occurred on 2006 February 12. These observations represent the first scientific results from the KIN, which operates in N band from 8 to 12.5 μm in a nulling mode. The nulling technique is the sparse aperture equivalent of the conventional coronagraphic technique used in filled aperture telescopes. In this mode the stellar light itself is suppressed by a destructive fringe, effectively enhancing the contrast of the circumstellar material located near the star. By fitting the unique KIN data, we have obtained an angular size of the mid-infrared continuum emitting material of 6.2, 4.0, or 5.4 mas for a disk profile, Gaussian profile (FWHM), and shell profile, respectively. The data show evidence of enhanced neutral atomic hydrogen emission and atomic metals including silicon located in the inner spatial regime near the white dwarf (WD) relative to the outer regime. There are also nebular emission lines and evidence of hot silicate dust in the outer spatial region, centered at ~17 AU from the WD, that are not found in the inner regime. Our evidence suggests that these features have been excited by the nova flash in the outer spatial regime before the blast wave reached these regions. These identifications support a model in which the dust appears to be present between outbursts and is not created during the outburst event. We further discuss the present results in terms of a unifying model of the system that includes an increase in density in the plane of the orbit of the two stars created by a spiral shock wave caused by the motion of the stars through the cool wind of the red giant star.