age of the open cluster. Extreme Population I stars belong to young open clusters. These are HII regions (see energetic processes) as they still contain much of the gas and dust of the original star-forming nebula. These clusters follow circular orbits and occur in the spiral arms of spiral...
Hertzsprung-Russell Diagram Data of Star Cluster CYG OB1starsCYG
The estimated age of the cluster is 17 ± 3 million years. In the study, the brightest star in the K-band that lay in the same line of sight as the cluster (St2-18) was given the identifier 1. The study concluded that the star likely had considerable infrared excess and may be a ...
We perform a detailed analysis of the HR diagram, taking proper account of the uncertainties and the effects of unresolved binaries, and derive ages and masses for the PMS stars. We find that the low-mass PMS stars have a mean age of about 5 Myr and show no evidence for a large age ...
Detailed characterization of these rare but precious globular cluster cataclysmics will yield valuable insights into the long-term evolution of CVs. Sign in to download full-size image Fig. 2. The HST/WFPC2 F336W (U) - F675W (R) color magnitude diagram of M80 (NGC 6093). T Sco ...
Spectrophotometric properties of pre-main sequence stars: the Epsilon Chamaeleontis cluster This result is consistent with Cha being the slightly younger PMS association, a few Myr younger according to the HertzsprungRussell (HR) diagram placement... Lyo A.-Ran,WA Lawson,MS Bessell - 《Monthly No...
I had spent the past several hours trying to figure out the mystery of the pointing. By now, only stragglers were sampling the field. Enough, I said, let me try a newer add on. The Stargate Asterism or Stargate Cluster is an asterism in the constellation Corvus consisting of six ...
By extension, this implies that mass, composition, and age do not uniquely specify the HR diagram location of pre-MS stars. 展开 关键词: stars: activity stars: evolution stars: pre-main sequence starspots DOI: 10.1088/0004-637X/807/2/174 ...
cluster have very nearly the same age and chemicalcomposition, the differences between the member stars are entirely the result of their different masses. As time progresses after the formation of a cluster, the massive stars, which evolve the fastest, gradually disappear from the cluster, becoming...
Hence, the interplay between the properties of the host star cluster (e.g., its escape velocity), those of the first-generation (1g) BBH population and the magnitude of the kick decides the maximum mass of a merger remnant in a given environment. This might be used to constrain the ...