Weighing the young stellar discs around Sgr A*

Sergei Nayakshin, Walter Dehnen, Jorge Cuadra, Reinhard Genzel

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55 Scopus citations


It is believed that young massive stars orbiting Sgr A* in two stellar discs on scales of ∼ 0.1-0.2 parsec were formed either farther out in the Galaxy and then quickly migrated inwards or in situ in a massive self-gravitating disc. Comparing N-body evolution of stellar orbits with observational constraints, we set upper limits on the masses of the two stellar systems. These masses turn out to be a few times lower than the expected total stellar mass estimated from the observed young high-mass stellar population and the standard galactic initial mass function (IMF). If these stars were formed in situ, in a massive self-gravitating disc, our results suggest that the formation of low-mass stars was suppressed by a factor of at least a few, requiring a top-heavy IMF for stars formed near Sgr A*.

Original languageEnglish
Pages (from-to)1410-1414
Number of pages5
JournalMonthly Notices of the Royal Astronomical Society
Issue number4
StatePublished - Mar 2006
Externally publishedYes


  • Accretion, accretion discs
  • Galaxies: active
  • Galaxy: centre
  • Stars: formation


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