The peculiar case of the “double-humped” super-luminous supernova SN 2006oz

SN 2006oz is a super-luminous supernova with a mysterious bright precursor that has resisted explanation in standard models.However,such a precursor has been predicted in the dual-shock quark nova model of super-luminous supernovae–the precursor is the supernova event while the main light curve of the super-luminous supernova is powered by the Quark-Nova（explosive transition of the neutron star to a quark star）.As the supernova is fading,the Quark-Nova re-energizes the supernova ejecta,producing a＂double-humped＂light curve.We show that the quark nova model successfully reproduces the observed light curve of SN 2006oz.     

大陆“弱”转换断层邻近的扩张与沉陷：以东非鲁夸裂谷为例

鲁夸裂谷为一长３００公里的半地堑盆地，它沿东非裂谷内长达１０００公里的大陆转换断层中段分布。盆地含有厚达１１公里的石炭系至第四系地层。尽管此边界断层以右旋走向滑动为主，盆地内最大扩张方向近垂直于该断层。但裂谷的扩张与沉陷不能以释放弯曲和斜向拉伸断几何形来解释。我们把这种扩张方向性解释为低磨擦，“弱”走滑边界断层的局部应力旋转特征。沿边界断面走向的磨擦强度差异控制着扩张的部位，垂直于裂谷边界断层的沉     

轻夸克物质团、奇异子和致密矮星

相对于核物质和奇异夸克物质, 仅由两味夸克构成的轻夸克物质(即ud夸克物质)有可能更稳定. 而对于由这三类物质构成的典型物质集团, 研究发现如果ud夸克物质具有较大的对称能, 那么其物质团会在特定大小(重子数$A\approx1000$)时最稳定. 在这种情况下, 就可能存在由ud夸克物质团和电子构成的致密矮星, 即ud夸克矮星. 通过进一步研究这类ud夸克矮星的结构可知: 相较于传统的由原子核和电子构成的白矮星, ud夸克矮星通常具有较小的半径, 而被正常物质覆盖的ud夸克矮星的半径则在它们之间, 这与最近观测到的质量和半径都异常小的白矮星相符.     

风帆训练舰,锻造海军栋梁

<正>甲午再现,120年前那场海战,我们是怎么败的?当时北洋海军组建时,李鸿章只忙于建立框架,而疏于构建精神。甲午战争的惨痛与耻辱,我们到底还记得没有?航海精神虚弱的民族如何能够抗衡百年来一直致力于海上侵略扩张的国家?我们该怎么办?只有我们强大,才会避免战争。当今世界局势,国家安定必须有军队的战略支撑,而海军是最重要的军事     

夏天高温与它的克星因子

通常在研究预报问题时,只考虑预报因子,而没有考虑预报的克星因子.本文以夏天高温为例,来说明它的克星因子,克星因子在预报问题中也是不可忽视的问题.     

Quark-Novae Ia in the Hubble diagram: implications for dark energy

The accelerated expansion of the Universe was proposed through the use of Type-Ia supernovae （SNe） as standard candles. The standardization depends on an empirical correlation between the stretch/color and peak luminosity of the light curves. The use of Type-Ia SNe as standard candles rests on the assumption that their properties （and this correlation） do not vary with redshift. We consider the possibility that the majority of Type-Ia SNe are in fact caused by a Quark-Nova detonation in a tight neutron-star-CO-white-dwarf binary system, which forms a Quark-Nova Ia （QN-Ia）. The spin-down energy injected by the Quark-Nova remnant （the quark star） contributes to the post-peak light curve and neatly explains the observed correlation between peak luminosity and light curve shape. We demonstrate that the parameters describing QN-Ia are NOT constant in redshift. Simulated QN-Ia light curves provide a test of the stretch/color correlation by comparing the true distance modulus with that determined using SN light curve fitters. We determine a correction between the true and fitted distance moduli, which when applied to Type-Ia SNe in the Hubble diagram recovers the ΩM = 1 cosmology. We conclude that Type-Ia SNe observations do not necessitate the need for an accelerating expansion of the Universe （if the observed SNe Ia are dominated by QNe Ia） and by association the need for dark energy.     

夸克物质与夸克星

二十世纪六七十年代强子结构研究的进展使人们认识到了亚核子--夸克--的存在,随后,实验和理论上关于夸克之间作用渐近自由性质的发现使学者们明确地提出了"夸克物质"的概念.理论上预言的这种物质是否真的存在将在很大程度上检验目前基本强作用的理论.夸克星就是夸克物质的可能存在形式之一,相关研究也是人们探索超核密度物质状态的重要途径,该文简述脉冲星、中子星及夸克星的研究历史,总结了近年来夸克物质与夸克星研究的重要成果,指出了夸克星与一般中子星的异同以及若干夸克星候选体.