The spectroscopic evolution of the recurrent nova T Pyxidis during its 2011 outburst - III. The ultraviolet development from iron curtain through the post-X-ray turnoff
The spectroscopic evolution of the recurrent nova T Pyxidis during its 2011 outburst - III. The ultraviolet development from iron curtain through the post-X-ray turnoff
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复发新星 T Pyxidis 在 2011 年爆发期间的光谱演化 - III。
DOI：
10.1051/0004-6361/201322545
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发表时间：
2014
影响因子：
6.5
通讯作者：
E. Sion
中科院分区：
文献类型：
--
作者：
I. D. G. Aquino;S. Shore;G. Schwarz;Elena Mason;S. Starrfield;E. Sion
我们将继续分析2011年爆发期间周期性新星T Pyx的多波长演化，重点关注1150-3000 nm区域的光谱发展。这个非凡的数据集提供了迄今为止任何新星（经典或复发）的最长时间基线紫外线高分辨率视图。观测涵盖了早期的铁幕阶段，当紫外线是完全光学厚，834天后发现时，爆发有效地结束。我们提出了一个分析的动力学和丰度的星际物种的共振线是在紫外线。Lyα分布在所有历元上都只与星际吸收相一致，并与H I 21 cm柱密度相一致。根据ISM的分析，到T Pyx的距离约为5 kpc。对于喷出物的演变，我们已经能够遵循电离和结构的变化，以前没有得到的分辨率和节奏。激发态等电子跃迁的C III，N IV]，和O V显示相同的分离吸收线的光学He I跃迁在光学最大值。这被解释为FUV基态线从300-1000 μ m范围内的喷射物内的共振吸收。所有物种的共振线都显示出在铁幕变得透明时（从第105天开始）在-1000到-3000 km s−1之间的吸收分量;这些吸收分量以相同的速度持续存在，并且从一个离子到另一个离子的强度变化到第834天。最后的紫外光谱，采取了超过800天后爆发，显示了相同的吸收线在NV和C IV作为第105天。没有证据表明存在星周吸收器。这一点和剖面演变的相关观测结果有效地排除了频谱的任何风模型。出现的图片是在视觉最大值之后变得光学薄的喷出物，因为X射线发射在向外传播的电离前沿之后变得可见，并且由于软X射线照射结束后喷出物膨胀，电离阶段冻结。
We continue the analysis of the multiwavelength evolution of the recurrent nova T Pyx during its 2011 outburst, focussing on the spectral development on the 1150–3000 Å region. This extraordinary data set presents the longest temporal baseline high resolution view of the ultraviolet for any nova to date (classical or recurrent). The observations cover the early Fe-curtain stage, when the UV was completely optically thick, to 834 days after discovery when the outburst was effectively over. We present an analysis of dynamics and abundances of the interstellar species whose resonance lines are accessible in the UV. The Lyα profile is consistent with only interstellar absorption at all epochs and agrees with the H I 21 cm column density. The distance obtained to T Pyx is about 5 kpc, based on the ISM analysis. For the ejecta evolution we have been able to follow the changes in ionization and structure with previously unobtained resolution and cadence. The excited state isoelectronic transitions of C III, N IV], and O V displayed the same detached absorption lines as the optical He I transitions during the optical maximum. This is explained as resonance absorption within the ejecta of FUV ground state lines from the 300–1000 Å range. The resonance lines of all species showed absorption components between –1000 and –3000 km s−1 as soon as the Fe-curtain turned transparent (from day 105); these persisted at the same velocities and varied in strength from one ion to another through day 834. The last ultraviolet spectrum, taken more than 800 days after outburst, showed the same absorption lines on N V and C IV as day 105. There was no evidence of circumstellar absorbers. This and the related observations of profile evolution effectively rule out any wind model for the spectrum. The picture that emerges is of ejecta that became optically thin after visual maximum as the X-ray emission became visible following an outwardly propagating ionization front and for which the ionization stages froze because of ejecta expansion after the end of the soft X-ray illumination.