The binary progenitor of Tycho Brahe's 1572 supernova

Ruiz‐Lapuente, P.; Comerón, F.; Méndez, J.; Canal, R.; Smartt, S. J.; Filippenko, A. V.; Kurucz, Robert L.; Chornock, R.; Foley, R. J.; Stanishev, V.; Ibata, Rodrigo

doi:10.1038/nature03006

Cited by 247 publications

(264 citation statements)

References 16 publications

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“…In the case of the 400 year old Tycho supernova remnant, we would expect to observe this surviving star. Nevertheless, no such object has been unambiguously identified (Ruiz-Lapuente et al 2004;Kerzendorf et al 2009;Schaefer & Pagnotta 2012). Some SNe and supernova remnants show evidence of interaction with circumstellar material which links them to the SD channel (Hamuy et al 2003;Chiotellis et al 2012;Dilday et al 2012).…”

Section: Introductionmentioning

confidence: 99%

Theoretical uncertainties of the Type Ia supernova rate

Claeys

Pols

Izzard

et al. 2014

A&A

280

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It is thought that Type Ia supernovae (SNe Ia) are explosions of carbon-oxygen white dwarfs (CO WDs). Two main evolutionary channels are proposed for the WD to reach the critical density required for a thermonuclear explosion: the single degenerate (SD) scenario, in which a CO WD accretes from a non-degenerate companion, and the double degenerate (DD) scenario, in which two CO WDs merge. However, it remains difficult to reproduce the observed SN Ia rate with these two scenarios. With a binary population synthesis code we study the main evolutionary channels that lead to SNe Ia and we calculate the SN Ia rates and the associated delay-time distributions. We find that the DD channel is the dominant formation channel for the longest delay times. The SD channel with helium-rich donors is the dominant channel at the shortest delay times. Our standard model rate is a factor of five lower than the observed rate in galaxy clusters. We investigate the influence of ill-constrained aspects of single-and binary-star evolution and uncertain initial binary distributions on the rate of Type Ia SNe. These distributions, as well as uncertainties in both helium star evolution and common envelope evolution, have the greatest influence on our calculated rates. Inefficient common envelope evolution increases the relative number of SD explosions such that for α ce = 0.2 they dominate the SN Ia rate. Our highest rate is a factor of three less than the galaxy-cluster SN Ia rate, but compatible with the rate determined in a field-galaxy dominated sample. If we assume unlimited accretion onto WDs, to maximize the number of SD explosions, our rate is compatible with the observed galaxy-cluster rate.

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Section: Introductionmentioning

confidence: 99%

Theoretical uncertainties of the Type Ia supernova rate

Claeys

Pols

Izzard

et al. 2014

A&A

280

326

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“…13 (see text). The location of Tycho G according to Kerzendorf et al (2009Kerzendorf et al ( , 2012 is shown with the error in black assuming a solar mass star with 5% error (Ruiz-Lapuente et al 2004) and an inclination angle of i = 60 • . The black square gives the location of Tycho G for an assumed inclination angle of i = 30 • .…”

Section: Comparison With Tycho Gmentioning

confidence: 99%

“…Tycho Brahe's SN 1572 is an SN Ia that exploded in the Milky Way. Ruiz-Lapuente et al (2004) have analyzed the stars within a circle of 0.65 arcmin radius of the center of the SNR up to an apparent visual magnitude V = 22. They found a star, Tycho G, similar to the Sun in surface temperature and luminosity, but with a lower surface gravity than an MS star.…”

Section: Introductionmentioning

confidence: 99%

Rotation of surviving companion stars after type Ia supernova explosions in the WD+MS scenario

Liu

Pakmor

Röpke

et al. 2013

A&A

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Context. In the single-degenerate (SD) scenario of type Ia supernovae (SNe Ia) the non-degenerate companion star survives the supernova (SN) explosion and thus should be visible near the center of the SN remnant and may show some unusual features. Therefore, a promising approach to test progenitor models of SNe Ia is to search for the companion star in historical SN remnants. Aims. Here we present the results of three-dimensional (3D) hydrodynamics simulations of the interaction between the SN Ia blast wave and a main-sequence companion taking into consideration its orbital motion and spin. The primary goal of this work is to investigate the rotation of surviving companion stars after SN Ia explosions in the WD+MS scenario. Methods. We used Eggleton's stellar evolution code including the optically thick accretion wind model to obtain realistic models of companion stars. The impact of the supernova blast wave on these companion stars was followed in 3D hydrodynamic simulations employing the smoothed particle hydrodynamics (SPH) code GADGET3. Results. We find that the rotation of the companion star does not significantly affect the amount of stripped mass and the kick velocity caused by the SN impact. However, in our simulations, the rotational velocity of the companion star is significantly reduced to about 14% to 32% of its pre-explosion value due to the expansion of the companion and because 55%−89% of the initial angular momentum is carried away by the stripped matter. Conclusions. Compared with the observed rotational velocity of the presumed companion star of Tycho's supernova, Tycho G, of ∼6 km s −1 , the final rotational velocity we obtain in our simulations is still higher by at least a factor of two. Whether this difference is significant and may cast doubts on the suggestion that Tycho G is the companion of SN 1572 has to be investigated in future studies. Based on binary population synthesis results, we present for the first time the expected distribution of rotational velocities of companion stars after the SN explosion, which may provide useful information for the identification of the surviving companion in observational searches in other historical SN remnants.

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“…Other attempts to constrain the progenitors have come from very detailed studies of the spectra of the supernovae 16,17 , and attempts have been made to search for the companion stars in supernova remnants 18 . We have taken a different approach by 3 searching for ways to directly detect the progenitor of a type Ia supernova in presupernova images of the position in the sky where the supernova occurred.…”

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confidence: 99%