Light-curve and spectral properties of ultrastripped core-collapse supernovae leading to binary neutron stars

Moriya, Takashi J.; Mazzali, Paolo A.; Tominaga, Nozomu; Hachinger, Stephan; Блинников, С. И.; Tauris, T. M.; Takahashi, Koh; Tanaka, Masaomi; Langer, N.; Podsiadlowski, Philipp

doi:10.1093/mnras/stw3225

Cited by 94 publications

(119 citation statements)

References 129 publications

(205 reference statements)

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“…Depending on the orbital separation and the mass of the helium star, an additional phase of mass transfer (Case BB RLO, Habets 1986;Tauris et al 2015) may be initiated. This stage of mass transfer is important since it enables a relatively long phase of accretion onto the NS, whereby the NS is recycled, and it allows for extreme stripping of the helium star prior to its explosion (as a so-called ultra-stripped SN, Tauris et al 2013Tauris et al , 2015Suwa et al 2015;Moriya et al 2017). Whether or not the system survives the second SN depends on the orbital separation and the kick imparted onto the newborn NS (Flannery & van den Heuvel 1975;Hills 1983;Tauris & Takens 1998).…”

Section: Résumé Of Dns Formationmentioning

confidence: 99%

“…Therefore, to enable an estimate of the expected kicks, it is necessary to calculate stellar density structures at the end of Case BB RLO evolutionary models (Tauris et al 2013. So far, however, these progenitor models have not been calculated selfconsistently to the very onset of core collapse (although see Moriya et al 2017, for a composite calculation model integrating two stellar evolution codes). In Wongwathanarat et al (2013), a formula is presented (see their eq.…”

Section: Ns Kick Magnitudes In Binariesmentioning

confidence: 99%

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Formation of Double Neutron Star Systems

Tauris

Krämer

Freire

et al. 2017

ApJ

640

690

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Double neutron star (DNS) systems represent extreme physical objects and the endpoint of an exotic journey of stellar evolution and binary interactions. Large numbers of DNS systems and their mergers are anticipated to be discovered using the Square-Kilometre-Array searching for radio pulsars and high-frequency gravitational wave detectors (LIGO/VIRGO), respectively. Here we discuss all key properties of DNS systems, as well as selection effects, and combine the latest observational data with new theoretical progress on various physical processes with the aim of advancing our knowledge on their formation. We examine key interactions of their progenitor systems and evaluate their accretion history during the high-mass X-ray binary stage, the common envelope phase and the subsequent Case BB mass transfer, and argue that the first-formed NSs have accreted at most ∼ 0.02 M ⊙ . We investigate DNS masses, spins and velocities, and in particular correlations between spin period, orbital period and eccentricity. Numerous Monte Carlo simulations of the second supernova (SN) events are performed to extrapolate pre-SN stellar properties and probe the explosions. All known close-orbit DNS systems are consistent with ultra-stripped exploding stars. Although their resulting NS kicks are often small, we demonstrate a large spread in kick magnitudes which may, in general, depend on the past interaction history of the exploding star and thus correlate with the NS mass. We analyze and discuss NS kick directions based on our SN simulations. Finally, we discuss the terminal evolution of close-orbit DNS systems until they merge and possibly produce a short γ-ray burst.

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Section: Résumé Of Dns Formationmentioning

confidence: 99%

Section: Ns Kick Magnitudes In Binariesmentioning

confidence: 99%

Formation of Double Neutron Star Systems

Tauris

Krämer

Freire

et al. 2017

ApJ

640

690

View full text Add to dashboard Cite

show abstract

“…Since the merger rate and merging time scale of binary compact objects still have uncertainties, it is important to constrain these values through future observations. Ultra-stripped supernova (SN) is a candidate for generation sites of binary compact objects, especially binary NSs (Tauris et al 2013(Tauris et al , 2015Moriya et al 2017). Ultra-stripped Type Ic SNe weakly explode and the destruction of the close binary system is expected to be suppressed (Suwa et al 2015).…”

Section: Introductionmentioning

confidence: 99%

“…Close binary systems forming ultra-stripped Type Ic SNe would also result in the very close system of compact objects so that the merger of these objects takes place within cosmic age (Tauris et al 2015). A fast-decaying faint Type Ic SN 2005ek (Drout et al 2013) is considered to belong to an ultra-stripped SN (Tauris et al 2013;Suwa et al 2015;Moriya et al 2017). Increasing observations of these SNe would constrain the merger rate and the merging period of the binary compact objects.…”

Section: Introductionmentioning

confidence: 99%

Explosive nucleosynthesis of ultra-stripped Type Ic supernovae: application to light trans-iron elements

Yoshida¹,

Suwa²,

Umeda³

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We investigate the explosive nucleosynthesis during two dimensional neutrino-driven explosion of ultra-stripped Type Ic supernovae evolved from 1.45 and 1.5 M ⊙ CO stars. These supernovae explode with the explosion energy of ∼ 10 50 erg and release ∼ 0.1 M ⊙ ejecta. The light trans-iron elements Ga-Zr are produced in the neutrinoirradiated ejecta. The abundance distribution of these elements has a large uncertainty because of the uncertainty of the electron fraction of the neutrino-irradiated ejecta. The yield of the elements will be less than 0.01 M ⊙ . Ultra-stripped supernova and core-collapse supernova evolved from a light CO core can be main sources of the light trans-iron elements. They could also produce neutron-rich nuclei 48 Ca. The ultrastripped supernovae eject 56 Ni of ∼ 0.006-0.01 M ⊙ . If most of neutrino-irradiated ejecta is proton-rich, 56 Ni will be produced more abundantly. The light curves of these supernovae indicate sub-luminous fast decaying explosion with the peak magnitude of about −15-−16. Future observations of ultra-stripped supernovae could give a constraint to the event rate of a class of neutron star mergers.

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“…A small amount of ejecta suggests that supernovae associated with double pulsar formation is fainter than normal core-collapse supernovae if the emission powered only by the radioactivity of 56 Ni and 56 Co (Tauris et al 2013;Suwa et al 2015;Moriya et al 2017). However, the spin-down power of new-born pulsars may be much higher than the radioactive power.…”

Section: Introductionmentioning

confidence: 99%

Rapidly Rising Optical Transients from the Birth of Binary Neutron Stars

Hotokezaka

Kashiyama

Murase

2017

ApJ

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We study optical counterparts of a new-born pulsar in a double neutron star system like PSR J0737-3039A/B. This system is believed to have ejected a small amount of mass of O(0.1M ⊙ ) at the second core-collapse supernova. We argue that the initial spin of the new-born pulsar can be determined by the orbital period at the time when the second supernova occurs. The spin angular momentum of the progenitor is expected to be similar to that of the He-burning core, which is tidally synchronized with the orbital motion, and then the second remnant may be born as a millisecond pulsar. If the dipole magnetic field strength of the nascent pulsar is comparable to that inferred from the current spin-down rate of PSR J0737-3039B, the initial spin-down luminosity is comparable to the luminosity of super-luminous supernovae. We consider thermal emission arising from the supernova ejecta driven by the relativistic wind from such a new-born pulsar. The resulting optical light curves have a rise time of ∼ 10 days and peak luminosity of ∼ 10 44 erg/s. The optical emission may last for a month to several months, due to the reprocessing of X-rays and UV photons via photoelectric absorption. These features are broadly consistent with those of the rapidly rising optical transients. The high spin-down luminosity and small ejecta mass are favorable for the progenitor of the repeating fast radio burst, FRB 121102. We discuss a possible connection between newborn double pulsars and fast radio bursts.

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Light-curve and spectral properties of ultrastripped core-collapse supernovae leading to binary neutron stars

Cited by 94 publications

References 129 publications

Formation of Double Neutron Star Systems

Formation of Double Neutron Star Systems

Explosive nucleosynthesis of ultra-stripped Type Ic supernovae: application to light trans-iron elements

Rapidly Rising Optical Transients from the Birth of Binary Neutron Stars

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