On quintessence star model and strange star
نویسندگان
چکیده
منابع مشابه
Rigidly Rotating Strange Quark Star
The possibility of the existence of quark matter dates back to early seventies. Bodmer remarked that matter consisting of deconfined up, down and strange quarks could be the absolute ground state of matter at zero pressure and temperature. If this is true then objects made of such matter, so-called ”strange star”, could exist. There are several proposed mechanisms for formation of quark stars. ...
متن کاملA strange star model for GRO J 1744 - 28
A model is suggested for the bursting x-ray pulsar, GRO J1744-28, where the compact object of the pulsar is proposed to be a strange matter star with crusts. It is suggested that two envelope crusts shield the two polar caps of an accreting strange stars owing to strong polar-cap magnetic fields. GRO J1744-28 might not have a unified crust, but two polar crusts. Bursts are the result of phase t...
متن کاملPsr 0943 + 10 : a Bare Strange Star ?
Recent work by Rankin & Deshpande strongly suggests that there exist strong " micro-storms " rotating around the magnetic axis of the 1.1s pulsar PSR 0943+10. Such a feature hints that most probably the large-voltage vacuum gap proposed by Ruderman & Sutherland (RS) does exist in the pulsar polar cap. However, there are severe arguments against the formation of the RS-type gap in pulsars, since...
متن کاملThe Fastest Rotating Pulsar : a Strange Star ?
According to the observational limits on the radius and mass, PSR 1937+21 is probably a strange star, or some neutron star equations of state should be ruled out, if we alternatively suggest that a dipole magnetic field (rather than a quadrupole one) is relevant to its radio emission. In order to find solid evidence to shown that PSR 1937+21 is a strange star, it is strongly suggested to measur...
متن کاملHow to identify a Strange Star
It has recently been shown, that the emission of gravitational radiation due to r-mode instabilities in hot, young neutron stars severely limits the rotation period of these stars [1–6]. Within the first year, where the star cools to 10K, the star will spin down to a few per cent of the Kepler-limit [7] (the ultimate rotation frequency where the stellar equator “falls off”), corresponding to a ...
متن کاملذخیره در منابع من
با ذخیره ی این منبع در منابع من، دسترسی به آن را برای استفاده های بعدی آسان تر کنید
ژورنال
عنوان ژورنال: The European Physical Journal C
سال: 2020
ISSN: 1434-6044,1434-6052
DOI: 10.1140/epjc/s10052-020-08433-6