Testing the white dwarf mass-radius relationship with eclipsing binaries
Testing the white dwarf mass-radius relationship with eclipsing binaries
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DOI：
10.1093/mnras/stx1522
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发表时间：
2017-06
影响因子：
4.8
通讯作者：
S. Parsons;B. Gänsicke;T. Marsh;R. Ashley;M. Bours;E. Breedt;M. Burleigh;C. Copperwheat;V. Dhillon;M. Green;L. Hardy;J. Hermes;P. Irawati;P. Kerry;S. Littlefair;M. Mcallister;S. Rattanasoon;A. Rebassa-Mansergas;D. Sahman;M. Schreiber
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文献类型：
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作者：
S. Parsons;B. Gänsicke;T. Marsh;R. Ashley;M. Bours;E. Breedt;M. Burleigh;C. Copperwheat;V. Dhillon;M. Green;L. Hardy;J. Hermes;P. Irawati;P. Kerry;S. Littlefair;M. Mcallister;S. Rattanasoon;A. Rebassa-Mansergas;D. Sahman;M. Schreiber
我们给出了分离的食双星中16颗白矮星的高精度、与模型无关的质量和半径测量，并将这些测量结果与以前发表的数据相结合，检验了理论上的白矮星质量-半径关系。我们达到了2.4%的质量和2.7%的半径的平均精度，最好的测量精度达到了0.3%的质量和0.5%的半径。我们发现，在大范围的质量和温度范围内，测量的半径和预测的半径之间有很好的一致性。我们还发现，所有质量小于0.48M⊙的白矮星的半径与氦核模型完全一致，但它们平均比碳-氧核模型的半径大9%。相比之下，质量大于0.52M⊙的白矮星的半径都与碳氧核模型一致。此外，我们还发现，除了一颗白矮星外，其余所有白矮星的半径都与具有较厚表面氢包层(10−5≥MH/≥10−4)的半径一致，这意味着这些白矮星的表面氢层不受共同包络演化的明显影响。
We present high-precision, model-independent, mass and radius measurements for 16 white dwarfs in detached eclipsing binaries and combine these with previously published data to test the theoretical white dwarf mass–radius relationship. We reach a mean precision of 2.4 per cent in mass and 2.7 per cent in radius, with our best measurements reaching a precision of 0.3 per cent in mass and 0.5 per cent in radius. We find excellent agreement between the measured and predicted radii across a wide range of masses and temperatures. We also find the radii of all white dwarfs with masses less than 0.48 M⊙ to be fully consistent with helium core models, but they are on average 9 per cent larger than those of carbon–oxygen core models. In contrast, white dwarfs with masses larger than 0.52 M⊙ all have radii consistent with carbon–oxygen core models. Moreover, we find that all but one of the white dwarfs in our sample have radii consistent with possessing thick surface hydrogen envelopes (10−5 ≥ MH/MWD ≥ 10−4), implying that the surface hydrogen layers of these white dwarfs are not obviously affected by common envelope evolution.