Star formation in the semistellar nucleus of M33

Details Star formation in the semistellar nucleus of M33 Star formation in the semistellar nucleus of M33

Apr 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983apj...267...80o&link_type=abstract

Astrophysical Journal, Part 1, vol. 267, Apr. 1, 1983, p. 80-92.

Astronomy and Astrophysics

Astrophysics

52

Galactic Nuclei, Metallicity, Spiral Galaxies, Star Distribution, Star Formation, Astronomical Models, Data Simulation, Early Stars, Globular Clusters, Stellar Color, X Ray Sources

Scientific paper

The author has performed a detailed spectral synthesis of high-precision spectrophotometry for the semistellar nucleus of M33, explicitly including metal-poor populations. He finds that ≡50% of the λ5050 light originates in stars younger than 1 Gyr. The youngest generation is ≡5×106 yrs old. The old population appears to have a metallicity [Fe/H] ≡ -0.5, in agreement with the metallicity-luminosity scale for E/S0 galaxies. Old, metal-poor models for M33's nucleus are astrophysically implausible. The mean star-formation rate in the nucleus over the past 1 Gyr has been ≡3×10-4 M_sun; yr-1, and the data suggest that star formation episodes are interrupted by intervals of ≡0.1 Gyr. The X-ray emission in the nucleus is unlikely to originate from a massive binary in the young population.

Affiliated with

Also associated with

No associations

Rating

Star formation in the semistellar nucleus of M33 does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Star formation in the semistellar nucleus of M33, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Star formation in the semistellar nucleus of M33 will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1233420