Quark-novae in binaries: Observational signatures and implications to astrophysics

Ouyed, Rachid; Leahy, D. A.; Koning, Nico; Staff, Jan E.

doi:10.1142/9789813226609_0197

Cited by 5 publications

(3 citation statements)

References 27 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The detailed PT process from baryons to quarks is not well understood. Olinto (1987) and Horvath & Benvenuto (1988) believed that the PT will last around 10 8 yr as a gradual process, while many researchers argued that the process might be a detonation mode with timescale from several milliseconds to ∼ 10 seconds (Cheng & Dai 1996;Ouyed et al 2002;Shu et al 2017;Prasad & Mallick 2018;Zhang et al 2018;Mariani et al 2019;Ouyed et al 2012Ouyed et al , 2019Singh et al 2020). Their studies show that the energy released during PT is compatible with a core collapse supernova (CCSN).…”

Section: Strange Star Scenariomentioning

confidence: 99%

A Strange Star Scenario for the Formation of Eccentric Millisecond Pulsar/Helium White Dwarf Binaries

Jiang

Dey

et al. 2015

ApJ

View full text Add to dashboard Cite

According to the recycling scenario, millisecond pulsars (MSPs) have evolved from low-mass X-ray binaries (LMXBs). Their orbits are expected to be circular due to tidal interactions during the binary evolution, as observed in most of the binary MSPs. There are some peculiar systems that do not fit this picture.Three recent examples are PSRs J2234+06, J1946+3417 and J1950+2414, all of which are MSPs in eccentric orbits but with mass functions compatible with expected He white dwarf companions. It has been suggested these MSPs may have formed from delayed accretion-induced collapse of massive white dwarfs, or the eccentricity may be induced by dynamical interaction between the binary and a circumbinary disk. Assuming that the core density of accreting neutron stars in LMXBs may reach the density of quark deconfinement, which can lead to phase transition from neutron stars to strange quark stars, we show that the resultant MSPs are likely to have an eccentric orbit, due to the sudden loss of the gravitational mass of the neutron star during the transition. The eccentricities can be reproduced with a reasonable estimate of the mass loss. This scenario might also account for the formation of the youngest known X-ray binary Cir X−1, which also possesses a low-field compact star in an eccentric orbit.

show abstract

Section: Strange Star Scenariomentioning

confidence: 99%

A Strange Star Scenario for the Formation of Eccentric Millisecond Pulsar/Helium White Dwarf Binaries

Jiang

Dey

et al. 2015

ApJ

View full text Add to dashboard Cite

show abstract

“…However, there are some physical phenomena that could mimic anti-glitches in timing data. Such phenomena include transfer of angular momentum from slower rotating crust to the faster crustal fluid (Thompson et al 2000), curling of magnetic lines (Lyutikov 2013), accretion of ambient matter (Katz 2009;Ouyed et al 2013), strong outburst (Tong 2013) and collision of small solid body with neutron star (Huang & Geng 2014). Of all these phenomena, none except the collision of small solid body with neutron star could produce a picture of anti-glitch with features of conventional glitch.…”

Section: Introductionmentioning

confidence: 99%

Microglitches in radio pulsars: the role of strange nuggets

Eya

Iyida

Urama

et al. 2020

Astrophys Space Sci

View full text Add to dashboard Cite

Strange Nuggets are believed to be among the relics of the early universe. They appear as dark matter due to their low charge-to-mass ratio. Their distribution is believed to be the same as that of dark matter. As such, they could be accreted by high magnetic field objects and their collisions with pulsars are inevitable. Pulsar glitches are commonly seen as sudden spin-ups in pulsar frequency. It is still an open debate with regard to mechanisms giving rise to such a phenomenon. However, there is a class of sudden changes in pulsar spin frequency known as microglitches. These event are characterized by sudden small change in pulsar spin frequency (δν/ν ≈ ±10 −9). Clearly, the negative signature seen in some of the events is inconsistent with the known glitch mechanisms. In this analysis, we suggest that accretion of strange nuggets with pulsars could readily give rise to microglitch events. The signature of the events depends on the energy of the strange nuggets and line of interaction.

show abstract

“…Confirming the QN as the engine driving LGRBs and FRBs means that other implications of QNe to cosmology (e.g., to re-ionization (Ouyed et al 2009c) and to type Ia SNe calibration (Ouyed et al 2014b)), to binary evolution (Ouyed et al 2016(Ouyed et al , 2018c and to AXPs/SGRs (e.g., Ouyed et al 2007aOuyed et al ,b, 2018d warrant further studies.…”

Section: Discussionmentioning

confidence: 95%

A quark nova in the wake of a core-collapse supernova: a unifying model for long duration gamma-ray bursts and fast radio bursts

Ouyed

Leahy

Koning

2020

Res. Astron. Astrophys.

View full text Add to dashboard Cite

By appealing to a Quark-Nova (QN; the explosive transition of a neutron star to a quark star) in the wake of a core-collapse Supernova explosion of a massive star, we develop a unified model for long duration Gamma-ray Bursts (LGRBs) and Fast Radio Bursts (FRBs). The time delay (years to decades) between the SN and the QN and, the fragmented nature (i.e. millions of chunks) of the relativistic QN ejecta are key to yielding a robust LGRB engine. In our model, a LGRB light-curve exhibits the interaction of the fragmented QN ejecta with a turbulent (i.e. filamentary and magnetically saturated) SN ejecta which is shaped by its interaction with an underlying pulsar wind nebula (PWN). The afterglow is due to the interaction of the QN chunks, exiting the SN ejecta, with the surrounding medium. Our model can fit BAT/XRT prompt and afterglow light-curves, simultaneously with their spectra, thus yielding the observed properties of LGRBs (e.g. the Band function and the X-ray flares). We find that the peak luminosity-peak photon energy relationship (i.e. the Yonetoku law), and the isotropic energy-peak photon energy relationship (i.e. the Amati law) are not fundamental but phenomenological. FRBs in our model result from coherent synchrotron emission (CSE) when the QN chunks interact with non-turbulent weakly magnetized PWN-SN ejecta, where conditions are prone to the Weibel instability. Magnetic field amplification induced by the Weibel instability in the shocked chunk frame sets the bunching length for electrons and pairs to radiate coherently. The resulting emission frequency, luminosity, duration and dispersion measure (DM) in our model are consistent with FRB data. We find a natural unification of high-energy burst phenomena from FRBs to LGRBs including X-ray Flashes (XRFs) and X-ray rich GRBs (XRR-GRBs) as well as Super-Luminous SNe (SLSNe). We find a possible connection between Ultra-High Energy Cosmic Rays and FRBs and propose that a QN following a binary neutron star merger can yield a short GRB (SGRB) with fits to BAT/XRT light-curves.

show abstract

Quark-novae in binaries: Observational signatures and implications to astrophysics

Cited by 5 publications

References 27 publications

A Strange Star Scenario for the Formation of Eccentric Millisecond Pulsar/Helium White Dwarf Binaries

A Strange Star Scenario for the Formation of Eccentric Millisecond Pulsar/Helium White Dwarf Binaries

Microglitches in radio pulsars: the role of strange nuggets

A quark nova in the wake of a core-collapse supernova: a unifying model for long duration gamma-ray bursts and fast radio bursts

Contact Info

Product

Resources

About