ВНИМАНИЕ! На форуме начался конкурс - астрофотография месяца ОКТЯБРЬ!
0 Пользователей и 1 Гость просматривают эту тему.
Альтернативность в том, что не требуется резкое и сильное (намного выше температуры плавления) нагревание.
намного выше температуры плавления
А что такое "эксорные вспышки"?
Насколько я понимаю, главной проблемой холодного диска является отсутствие понимания того, каков физический механизм слипания холодных пылинок между собой. За счёт чего закристаллизовавшаяся капелька прилепляется к матрице? Опять за счёт электростатических сил?
https://en.wikipedia.org/wiki/EX_Lupi
The baseline hypothesis for models that are linked to the early active Sun, as well as most models that lie in the realm of purely hypothesized, is that chondrules were free-floating wanderers within an environment in the protoplanetary disk. Since this assumption underlies most interpretations of chondrules, it has become a canonical, or well-accepted, viewpoint. Chondrule formation is, in the meteorite and cosmochemistry community, traditionally linked to planet formation in that chondrules are thermally processed before they are accreted to small asteroids and thus the process that formed them is a step toward forming planets.
The very existence of chondrules presents us with some fundamental questions about the origin of the solar system and formation of the planets. The simple and obvious problem is that we would like to know how chondrules formed. This is more than just an intriguing, unsolved scientific puzzle. If we knew how chondrules formed, we would have a greater understanding of whether chondrules played an essential and formative role in planet formation or whether they are insignificant by-products of a common process such as collisions between planetesimals and planetary embryos. Chondrule formation models have made significant progress recently. Several models now successfully address the first-order constraints of thermal histories that chondrule observations require. However, some of these models rely on processes that are predicted but are not known to have occurred within the protoplanetary disk environment, so that they remain hypothetical. The challenge for chondrule formation models is to advance to the level in which they address second- and third-order constraints that must also be satisfied for a successful solution.