致密星并合(中子星－中子星并合与中子星－黑洞并合)后抛射出的富中子(neutron rich)物质是合成r过程元素(r-process elements)的重要场所之一，近17年来的理论研究认为，这些r过程元素衰变产生的能量在热化后将形成光学－近红外(Optical－NIR)辐射，这种光学－近红外暂现现象被称为“Li-Paczy´nski 新星(Li-Paczy´nski novae)”，简称为“LP新星”，由于它们的典型峰值亮度约为典型的新星(novae)亮度的1000倍，因此又被称为“千新星(Kilonovae)”。此外，理论与观测都直接或间接地表明致密星并合在一定条件下会形成持续时间较短(T90.2 s)的伽玛射线暴(简称短暴，SGRBs)，且大部分短暴可能源自致密星并合。在短暴的余辉被确定后，人们就致力于搜寻伴随短暴的LP新星。介绍近17年来LP新星的理论进展。%Neutron rich matter ejected after compact ob ject merger (neutron star-neutron star merger and neutron star-black hole merger) provides one of the most important environ-ments of syntheses of r-process elements. In recent seventeen years, theoretical studies have proposed that heat produced during the decay of r-process elements can produce optical/near infrared radiation after thermalization. This type of optical/near infrared transients is called Li-Paczy´nski novae, or LP-novae for short. Since the typical peak luminosity of LP-novae is∼1000 times brighter than that of typical novae, they are also called Kilonovae. Besides, both theoretical and observational studies have showed, directly or indirectly, that under certain conditions, compact object mergers can produce short gamma-ray bursts (SGRBs for short, T90 . 2 s), and most SGRBs may come from compact ob ject mergers. After the identification of SGRB afterglows, dedicated searches of LP-novae from SGRBs have been taken. In this review we present the theoretical progress of LP-novae. Observational aspect will appear in the upcoming paper.
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