THE EXPANDING BIPOLAR SHELL OF THE HELIUM NOVA V445 PUPPIS
THE EXPANDING BIPOLAR SHELL OF THE HELIUM NOVA V445 PUPPIS
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DOI：
10.1088/0004-637x/706/1/738
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发表时间：
2009-10
期刊：
影响因子：
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通讯作者：
P. Woudt;D. Steeghs;D. Steeghs;M. Karovska;B. Warner;B. Warner;P. J. Groot;G. Nelemans
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文献类型：
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作者：
P. Woudt;D. Steeghs;D. Steeghs;M. Karovska;B. Warner;B. Warner;P. J. Groot;G. Nelemans
从多历元自适应光学成像和积分场单位光谱学，我们报告了氦新星V445船尾座（Nova Puppis 2000）周围的膨胀和狭窄限制的双极壳层的发现。一个赤道尘埃盘遮住了新星遗迹，外流的特征是极区外流速度很大，为6720 ± 650 km s−1，而结的运动速度更大，为8450 ± 570 km s−1。我们推导出膨胀视差距离为8.2 ± 0.5 kpc，并推导出爆发前的亮度为log L/L返= 4.34 ± 0.36。由此得出的光度表明船尾座V445可能包含一颗大质量的白色矮星，该矮星从一颗星星上高速吸积，使其成为双星群体的一部分，由于大质量的白色矮星表面积累了丰富的氦物质，可能导致超新星Ia爆炸。
From multi-epoch adaptive optics imaging and integral field unit spectroscopy, we report the discovery of an expanding and narrowly confined bipolar shell surrounding the helium nova V445 Puppis (Nova Puppis 2000). An equatorial dust disc obscures the nova remnant, and the outflow is characterized by a large polar outflow velocity of 6720 ± 650 km s−1 and knots moving at even larger velocities of 8450 ± 570 km s−1. We derive an expansion parallax distance of 8.2 ± 0.5 kpc and deduce a pre-outburst luminosity of the underlying binary of log L/L☉ = 4.34 ± 0.36. The derived luminosity suggests that V445 Puppis probably contains a massive white dwarf accreting at high rate from a helium star companion making it part of a population of binary stars that potentially lead to supernova Ia explosions due to accumulation of helium-rich material on the surface of a massive white dwarf.