80 research outputs found
Strangeon Stars
Stable micro-nucleus is 2-flavored (u and d), whereas stable macro-nucleus
could be 3-flavored (u, d and s) if the light flavor symmetry restores there.
Nucleons are the constituent of a nucleus, while strangeons are named as the
constituent of 3-flavored baryonic matter. Gravity-compressed baryonic object
created after core-collapse supernova could be strangeon star if the energy
scale (~0.5 GeV) cannot be high enough for quark deconfinement and if there
occurs 3-flavor symmetry restoration. Strangeon stars are explained here,
including their formation and manifestation/identification. Much work, coupled
with effective {micro-model} of strangeon matter, is needed to take advantage
of the unique opportunities advanced facilities will provide.Comment: submitted to Proceedings of QCS2017, 20-22 Feb 2017, YITP, Japa
To differentiate neutron star models by X-ray polarimetry
The nature of pulsar is still unknown because of non-perturbative effects of
the fundamental strong interaction, and different models of pulsar inner
structures are then suggested, either conventional neutron stars or quark
stars. Additionally, a state of quark-cluster matter is conjectured for cold
matter at supranuclear density, as a result pulsars could thus be quark-cluster
stars. Besides understanding different manifestations, the most important issue
is to find an effective way to observationally differentiate those models.
X-ray polarimetry would play an important role here. In this letter, we focus
on the thermal X-ray polarization of quark/quark-cluster stars. While the
thermal X-ray linear polarization percentage is typically higher than ~10% in
normal neutron star models, the percentage of quark/quark-cluster stars is
almost zero. It could then be an effective method to identify
quark/quark-cluster stars by soft X-ray polarimetry. We are therefore expecting
to detect thermal X-ray polarization in the coming decades.Comment: 4 pages, 3 figures, submitte
Strangeon Matter in a Liquid Drop Model
The liquid drop model of 2-flavored ( and ) nucleus is well known and
successful, analogically, a similar drop model for 3-flavored (, and
) nucleus is developed. A 3-flavored nucleus conjectured could be stable
only if its baryon number is lager than a critical one, , in which
strangeons are the constituent as an analogy of nucleons for nucleus. We try to
model strangeon matter in a sense of phenomenological liquid drop, with two
free parameters: the mass per bayron of a strangeon in vacuum, , and
potential deep between strangeons, . It is found that, for
GeV and MeV, strangeon matter could be stable and its
critical number could be as low as .Comment: submitted to Proceedings of QCS2017, 20-22 Feb 2017, YITP, Japa
Two types of glitches in a solid quark star model
Glitch (sudden spinup) is a common phenomenon in pulsar observations.
However, the physical mechanism of glitch is still a matter of debate because
it depends on the puzzle of pulsar's inner structure, i.e., the equation of
state of dense matter. Some pulsars (e.g., Vela-like) show large glitches
({\Delta}{\nu}/{\nu}~10^-6) but release negligible energy, whereas the large
glitches of AXPs/SGRs (anomalous X-ray pulsars/soft gamma repeaters) are
usually (but not always) accompanied with detectable energy releases
manifesting as X-ray bursts or outbursts. We try to understand this aspect of
glitches in a starquake model of solid quark stars. There are actually two
kinds of glitches in this scenario: bulk-invariable (Type I) and bulk-variable
(Type II) ones. The total stellar volume changes (and then energy releases)
significantly for the latter but not for the former. Therefore, glitches
accompanied with X-ray bursts (e.g., that of AXP/SGRs) could originate from
Type II starquakes induced probably by accretion, while the others without
evident energy release (e.g., that of Vela pulsar) would be the result of Type
I starquakes due to, simply, a change of stellar ellipticity.Comment: 6 pages, 2 figures, accepted for publication in MNRA
Supernova Neutrino in a Strangeon Star Model
The neutrino burst detected during supernova SN1987A is explained in a
strangeon star model, in which it is proposed that a pulsar-like compact object
is composed of strangeons (strangeon: an abbreviation of "strange nucleon"). A
nascent strangeon star's initial internal energy is calculated, with the
inclusion of pion excitation (energy around 10^53 erg, comparable to the
gravitational binding energy of a collapsed core). A liquid-solid phase
transition at temperature ~ 1-2 MeV may occur only a few ten-seconds after
core-collapse, and the thermal evolution of strangeon star is then modeled. It
is found that the neutrino burst observed from SN 1987A could be re-produced in
such a cooling model.Comment: 15 pages, 7 figures, 1 tabe
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