Pure hadronic compact stars, above a threshold value of their gravitational mass (central pressure), are metastable to the conversion to quark stars (hybrid or strange stars). In this paper, we present a systematic study of the metastability of pure hadronic compact stars using different relativistic models for the equation of state (EoS). In particular, we compare results for the quark-meson coupling (QMC) model with those for the Glendenning--Moszkowski parametrization of the non-linear Walecka model (NLWM). For QMC model, we find large values ($M_{cr} = 1.6$ -- $1.9 M_\odot$) for the critical mass of the hadronic star sequence and we find that the formation of a quark star is only possible with a soft quark matter EoS. For the Glendenning--Moszkowski parametrization of the NLWM, we explore the effect of different hyperon couplings on the critical mass and on the stellar conversion energy. We find that increasing the value of the hyperon coupling constants shifts the bulk transition point for quark deconfinement to higher densities, increases the stellar metastability threshold mass and the value of the critical mass, and thus makes the formation of quark stars less likely. For the largest values of the hyperon couplings we find a critical mass which may be as high as 1.9 - 2.1 $M_\odot$. These stellar configurations, which contain a large central hyperon fraction ($f_{Y,cr} \sim 30 %$), would be able to describe highly-massive compact stars, such as the one associated to the millisecond pulsars PSR B1516+02B with a mass $M = 1.94^{+ 0.17}_{- 0.19} M_{\odot}$.
Cosmic rays V. The nonthermal radio emission of the old nova GK Per - a signature of hadronic interactions?
利用Biermann（1993）和Biermann and Cassinelli（1993）提出的星风激波中粒子加速模型，我们证明了激变变星GK Per的非热射电发射光谱可以得到一致的解释。我们认为射电谱是由强子次级电子/正电子产生的，在光学薄的情况下，它们给出的特征射电谱的谱指数比最大值低+1/3，而在风速比激波速度慢的情况下，其谱指数比最大值高-0.7。我们测试所提出的概念与OB和沃尔夫拉叶星以及射电超新星的无线电数据的一致性。有一些证据表明，这一过程是重要的射电辐射从活动星系核，无论是在紧凑的和扩展的发射。我们认为，这样的无线电频谱是一个独特的特征强子相互作用。
On the nature of bimodal initial velocity distribution of neutron stars
我们认为射电星反冲速度分布的双峰性质与强子星（{ \it，即}）之间的二分法有关。不含夸克物质的中子星）和夸克星。双峰性可能是由于不同的爆炸机制导致形成两种类型的致密星，或者由于两组不同的参数掌握了一种特定的反冲机制。低速最大值（在$\sim 100$ km s $^{-1}$）与强子星的形成有关，而第二个峰值对应于夸克星。在强子星延迟坍缩为夸克星的模型中（Berezhiani et al. 2003 \nocite{bbd2003}），夸克解除禁闭导致了第二次能量释放和第二次反冲，除了在超新星爆炸过程中给予新形成的强子星的反冲之外。如果电磁火箭机制对脉冲星反冲有重要贡献，那么高速度峰值可能与夸克星相对于强子星的较短初始自旋周期有关。我们讨论这些场景的{ \it proet contra}。
