The Importance of the Mass of First-Generation Stars
Signatures of First Stars Recorded by Low-Mass Milky-Way Stars
Discovery of a Low-Mass Star with Unique Chemical Abundance Ratios
Rather, explosion models of very-massive stars can explain both the relatively high abundance ratio of iron as well as the low abundances of lighter elements (Fig. 3). This means that this star most likely preserves the elemental abundance ratios produced by a first-generation very-massive star.
Impact of this Study
- The JSPS Grants-in-Aid for Scientific Research (23224004)
- Grant PHY 08-22648: Physics Frontiers Center/Joint Institute for Nuclear Astrophysics (JINA), awarded by the U.S. National Science Foundation.
- Wako Aoki (National Astronomical Observatory of Japan)
- Nozomu Tominaga (Konan University & Kavli IPMU [WPI], University of Tokyo)
- Timothy C. Beers (University of Notre Dame)
- Satoshi Honda (University of Hyogo)
- Young Sun Lee (New Mexico State University)
A single low-energy, iron-poor supernova as the source of metals in the star SMSS J031300.36−670839.3
Figure 5: Artist's rendition of new generations of stars. The material that included heavy elements from the first-generation, very-massive stars mixed with hydrogen around the star. New generations of stars formed from the gas clouds that included small amount of heavy elements. SDSS J0018-0939, a low-mass star with a long lifetime, formed as one of these second-generation stars, recording the products of a first-generation very-massive star. (Credit: NAOJ)