After the LP-Nova models have been proposed and short gamma-ray burst (SGRB) afterglows have been discovered, dedicated searches for LP-Novae from SGRB opti-cal (and near-infrared) afterglows have been actively carried on. In this paper, we summarize these observational progresses until 2012 in the first part. In the second part, we conclude the basic properties of GRBs 130603B and 060614 as well as the theoretical interpretations for their optical-near infrared counterparts whose near infrared excess can be indicative of the signatures of LP-Novae. In the third part, we conclude the basic properties of GRB 080503 and the theoretical interpretations for its optical and X-ray counterparts whose lightcurves can be decomposed into two components originated from afterglow emission and the ejecta heated by a magnetar leaved after double neutron star merger, the latter is nicknamed “Merger-Nova”. If the interpretations for the SGRB-associated optical−infrared counter-parts are correct, they may provide the first direct evidences showing that short bursts are from compact star mergers and some special long bursts are also from compact star mergers. Besides LP-Novae (and Merger-Novae), the high speed orbital motions of the compact binary just before the merger as well as the merger itself can produce strong Gravitational-Wave Bursts (GWBs). As the era of gravitational wave detection comes soon, the theoretical stud-ies and observational searches of the electromagnetic counterparts of neutron star-neutron star or neutron star- black hole mergers have received more attentions. Since the gravita-tional wave positioning has larger uncertainty, observation of the associated LP-Novae can be the best way to precisely locate the GWB. The fast-developing high-cadence wide-field opti-cal-near infrared surveys will explore transients such as LP-Novae efficiently, and mutually promote gravitational wave detections and studies. Therefore, in the last part we present the methods for future searches of LP-Novae, and the prospect of the multi-messenger detections.%在Li-Paczynski 新星(LP新星)模型被提出以及短暴的余辉被确认后，人们就积极地在短暴的光学(或光学－近红外)对应体中寻找LP新星存在的证据。第2章总结2013年之前的观测结果。第3、4章分别介绍短暴GRB 130603B、GRB 060614的基本性质与它们的近红外对应体的解释，它们的近红外超可能是LP 新星存在的信号。第5章介绍短暴GRB 080503的基本性质以及它的光学对应体与X射线对应体的解释，它的光学与X射线光变曲线的晚期再增亮被解释为中子星并合之后的磁星加热的喷射物辐射(Merger-Nova辐射)。如果对于以上短暴伴随的光学－近红外对应物的解释正确，那么它们就给出了短暴与一些特殊的长暴来自致密星并合的第一批证据。除产生LP新星(与Merger-Novae)外，致密星并合之前的高速轨道运动与并合自身都将产生强烈的引力波暴(Gravitational-Wave Bursts, GWBs)。随着引力波时代的到来，致密星并合对应的各种电磁波现象的理论研究与观测受到更加密集的关注。由于引力波暴定位的不确定性较大，因此伴随引力波暴的LP新星可以作为引力波暴精确定位的最佳候选者之一。正在快速发展的高频度宽场光学－近红外巡天将对LP新星等现象进行富有成效的探索，并与引力波探测研究互相影响。因此，我们在最后介绍未来探测LP新星的方法及其多信使探测的前景。
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