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: http://star.arm.ac.uk/highlights/2012/615.html
Дата изменения: Wed Sep 26 17:15:24 2012 Дата индексирования: Tue Oct 2 03:19:33 2012 Кодировка: IBM-866 Поисковые слова: jupiter |
Chen, X., Jeffery, C. S., Zhang, X., Han, Z.
Figure 1: Left panel: constraints on the progenitors of SNe Ia of double CO WDs in the M1–M2 plane. The black lines are contours of the ejected mass fraction 1 тИТ β with values of, from left to right, 0.0, 0.1, … and 0.9, respectively. The red lines mark contours of merger mass M1 + M2 = Mch (conservative case, solid line), M1 + βM2 = Mch (non-conservative, dotted line), and M1 + β(t)M2(t)dt = Mch (non-conservative, dashed line). The vertical lines give the boundaries for M1 = 0.9 and 1.0 M☉. The areas to the right of each color line represent M ≥ Mch and hence DD SN Ia progenitor candidates under the corresponding constraints. Right panel: CO DDs from our population synthesis with M1 + M2 > Mch which can merge within a Hubble time; the blue dots have mass ratios q = M2 /M1 ≥ 2/3. The black dash-dot-dot-dotted line shows the boundary of q = 2/3, and the red lines are the same as those in the left-hand panel.
Abstract
Recent theoretical and observational studies both argue that the merging of double carbon-oxygen white dwarfs (WDs) is responsible for at least some Type Ia supernovae (SNe Ia). Previous (standard) studies of the anticipated SN birthrate from this channel have assumed that the merger process is conservative and that the primary criterion for explosion is that the merged mass exceeds the Chandrasekhar mass. Han & Webbink demonstrated that mass transfer and merger in close double WDs will in many cases be non-conservative. Pakmor et al. further suggested that the merger process should be violent in order to initiate an explosion. We have therefore investigated how the SN Ia birthrate from the double-degenerate (DD) channel is affected by these constraints. Using the binary-star population-synthesis method, we have calculated the DD SN Ia birthrate under conservative and non-conservative approximations, and including lower mass and mass-ratio limits indicated by recent smoothed-particle-hydrodynamic calculations. The predicted DD SN Ia rate is significantly reduced by all of these constraints. With dynamical mass loss alone (violent merger) the birthrate is reduced to 56% of the conservative rate. Requiring the mass ratio q > 2/3 further reduces the birthrate to 18% that of the standard assumption. An upper limit of 0.0061 SNuM, or a Galactic rate of 4.6 †Ч 10тИТ4 yrтИТ1, might be realistic.
Last Revised: 2012 September 26th |