"सूर्य": अवतरणों में अंतर

|bibcode = 2005Natur.436.1127B }}</ref> प्राचीन [[उल्कापिंड | उल्कापिंडों]] के अध्ययन अल्पजीवी आइसोटोपो के स्थिर नाभिक के निशान उजागर करते है, जैसे कि [[लौह-60]], जो केवल विस्फोटित, अल्पजीवी तारों में निर्मित होता है | Studies of ancient [[meteorite]]s reveal traces of stable daughter nuclei of short-lived isotopes, such as [[iron-60]], that form only in exploding, short-lived stars. This indicates that one or more supernovae must have occurred near the location where the Sun formed. A [[shock wave]] from a nearby supernova would have triggered the formation of the Sun by compressing the gases within the molecular cloud and causing certain regions to collapse under their own gravity.<ref>{{cite doi|10.1080/00107511003764725 }}</ref> As one fragment of the cloud collapsed it also began to rotate due to [[conservation of angular momentum]] and heat up with the increasing pressure. Much of the mass became concentrated in the center, while the rest flattened out into a disk which would become the planets and other solar system bodies. Gravity and pressure within the core of the cloud generated a lot of heat as it accreted more gas from the surrounding disk, eventually triggering [[stellar nucleosynthesis|nuclear fusion]]. Thus, the Sun was born.