Radii and Mass-loss Rates of Type IIb Supernova Progenitors

Abstract

Several Type IIb supernovae (SNe IIb) have been extensively studied, both in terms of the progenitor radius and the mass-loss rate in the final centuries before the explosion. While the sample is still limited, evidence has been accumulating that the final mass-loss rate tends to be larger for a more extended progenitor, with the difference exceeding an order of magnitude between the more and less extended progenitors. The high mass-loss rates inferred for the more extended progenitors are not readily explained by a prescription commonly used for a single stellar wind. In this paper, we calculate a grid of binary evolution models. We show that the observational relation in the progenitor radii and mass-loss rates may be a consequence of non-conservative mass transfer in the final phase of progenitor evolution without fine tuning. Further, we find a possible link between SNe IIb and SNe IIn. The binary scenario for SNe IIb inevitably leads to a population of SN progenitors surrounded by dense circumstellar matter (CSM) due to extensive mass loss (Ṁ 10 −4 M ⊙ yr −1 ) in the binary origin. About 4 % of all observed SNe IIn are predicted to have dense CSM, produced by binary non-conservative mass transfer, whose observed characteristics are distinguishable from SNe IIn from other scenarios. Indeed, such SNe may be observationally dominated by systems experiencing huge mass loss in the final 10 3 yr, leading to luminous SNe IIn or initially bright SNe IIP or IIL with a characteristics of SNe IIn in their early spectra.

Ultraviolet Detection of the Binary Companion to the Type IIb SN 2001ig

“…, when averaged over the final 1000 years before the SN explosion (Ouchi & Maeda 2017), which is comparable to that inferred from the radio observations for SN 2001ig (Ryder et al 2004). The CSM produced by the binary interaction could be the cause of the observed He II λ4686 feature discussed in Section 3.2.…”

“…This particular BPASS model terminates with a primary core mass of ∼3.5 M e and with ∼0.04M e of H remaining. These numbers are quite similar to those yielded by the independent binary evolution models of Ouchi & Maeda (2017) for a secondary-to-primary mass ratio of 0.6<q<0.8, initial orbital period 200<P<600 days, and a low efficiency ( f≈0) of mass accretion from the primary onto the secondary. The blue loop in Figure 3 is similar to that seen in the models of Yoon et al (2017) for TypeIIb interacting binary progenitors with periods of a few hundred days, and masses closer to 10M e than 20M e .…”

The expansion of stripped-envelope stars: Consequences for supernovae and gravitational-wave progenitors

“…Götberg et al 2017Götberg et al , 2018. At low metallicity, Yoon et al (2010Yoon et al ( , 2017, Claeys et al (2011), andOuchi &Maeda (2017) show that the amount of hydrogen left at the surface of the donor star is a function of the initial orbital separation. In appendix C, we demonstrate that, for case B mass transfer, our general findings are robust against variations of the orbital period at low metallicity.…”

Upper limits on very-high-energy gamma-ray emission from core-collapse supernovae observed with H.E.S.S.

“…Note that type II objects can also exhibit enhanced pre-SNe mass-loss rates above 10 −3 M yr −1 (e.g. Das & Ray 2017;Arcavi et al 2017), and other studies have shown that such high mass-loss rates are not so rare among type IIb SNe (Fuller 2017;Ouchi & Maeda 2017). It is then reasonable to expect ∼1 to 2 cc-SNe withṀ > 10 −4 M yr −1 occurring per year, within a radius of 18 Mpc, whatever the sub-type.…”