THE HIGH-MASS STELLAR INITIAL MASS FUNCTION IN M31 CLUSTERS
نویسندگان
چکیده
منابع مشابه
The Stellar Initial Mass Function
The current status of both the observational evidence and the theory of the stellar initial mass function (IMF) is reviewed, with particular attention to the two basic, apparently universal features shown by all observations of nearby stellar systems: (1) a characteristic stellar mass of the order of one solar mass, and (2) a power-law decline of the IMF at large masses similar to the original ...
متن کاملI. the Stellar Initial Mass Function
o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o oo o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o We summarize recent bservati nal and the retical pr gress aimed at understanding the rigin f the stellar initial mass functi n (IMF), with specific f cus n galactic star-f rming regi ns. We synthesize data fr m vari us eff rts t determine the IMF in very y...
متن کاملThe Stellar Initial Mass Function and Beyond
A brief review is given of the basic observed features of the stellar IMF, and also of some of the theoretical ideas and simulations that may help to explain these features. The characteristic stellar mass of order one solar mass may derive from the typical masses of the observed starforming clumps in molecular clouds, and the typical clump mass may in turn be determined mainly by the Jeans mas...
متن کاملUnderstanding the Stellar Initial Mass Function
The essential features of the stellar Initial Mass Function are, rather generally, (1) a peak at mass of a few tenths of a solar mass, and (2) a power-law tail toward higher masses that is similar to the original Salpeter function. Recent work suggests that the IMF peak reflects a preferred scale of fragmentation associated with the transition from a cooling phase of collapse at low densities t...
متن کاملModeling a high mass turn down in the stellar initial mass function
Statistical sampling from the stellar initial mass function (IMF) for all star-forming regions in the Galaxy would lead to the prediction of ∼ 1000 M⊙ stars unless there is a rapid turn-down in the IMF beyond several hundred solar masses. Such a turndown is not necessary for dense clusters because the number of stars sampled is always too small. Although no upper mass limits to star formation h...
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ژورنال
عنوان ژورنال: The Astrophysical Journal
سال: 2015
ISSN: 1538-4357
DOI: 10.1088/0004-637x/806/2/198