Analysis and Possible Methods of Detection of Quark Stars

The observation of events like GW170817 have provided enormous opportunities and data to study many celestial objects. Among these infinite celestial objects, today we discuss and provide theoretical analysis and possible methods of detection of Quark Stars.


Introduction and Analysis
Multiple scientists like Bodmer (1971) have pointed out theoretical possibility of presence of quark matter and its composition of up, down and strange quarks.This startling theory provide possibilities about superdense matter and if verified by future technologies, would change our understanding of early universe, and cosmology itself. When the degeneracy pressure inside a neutron star is surpassed, and at extreme temperature and pressure, the neutrons undergo deconfinement transitions to a new phase of quarks inside the star as observed in heavy-ion collision. This creates an ultra dense phase of quark matter, and the star is called a Quark star.
Though the equation of state (EoS) of a quark star might not be completely certain at this time, this analysis will provide theoretical evidence about their existence.
A localised assembly of quark-gluon in chemical equilibrium is termed at QGP and is believed to be filled throughout the space during early stages of the universe. The theory predicting deconfinement transition to QGP [1] is termed as quantum chromodynamics or QCD.
Integrating astrophysical observations and theoretical ab initio calculations, we observe that neutron stars with mass similar to 1.4 times the solar mass exhibit this deconfined state, QGP properties of the star. Another type of modes we will be using will be g modes or gravitational modes. If density discontinuity exists inside a neutron star about to be transitioned, due to the presence of a quark core, the detection of g mode would verify the results. These mainly arise due to smoothening of material inhomogeneities along equipotential level surfaces. They differ from pressure or p modes interim of their tangential displacement being much bigger than radial displacement. The g mode is dependent on amplitude of discontinuity. Another metric: color-superconductivity lowering transition pressure, shows hybrid stars with di-quark cores.
The previous results hold for non rotating objects [4]. However, the observations show at least some degree of rotation in all neutron stars whether transitioning or not. Rotating compact objects are influenced by non axisymmetric dynamical and secular instabilities. But in practice, very young proto-neutron stars are impacted by differential rotations. Secular instabilities, which require dissipation due, are associated with large currents coupled to gravitational radiation. This viscous damping makes the star stable at low frequencies. These findings establish our last base of detection. Future studies solving multiple base equations mentioned in the studies could find a numerical equation or data corresponding to a quark star and confirm its presence in the universe.
Analysis and Possible Methods of Detection of Quark Stars 7

Suggestions for future studies
With better theoretical understanding, to confirm quark stars, studies in the field of gravitational instabilities due to rotational with statistical emphasis and limit on rotation posed by mass loss at the equator should be promoted.

Conclusion
With advancing technologies and large projects like NICER and advanced LIGO/Virgo in cosmology and new statistical data continuously being recorded by them, we are very close to confirming quark stars. This paper presented an overview analysis of cosmology studies related to quark stars, and provided adapted versions of their possible detections.