期刊
SCIENCE
卷 347, 期 6226, 页码 1126-1128出版社
AMER ASSOC ADVANCEMENT SCIENCE
DOI: 10.1126/science.1259063
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资金
- W. M. Keck Foundation
- NASA through the Planetary Science Division of the NASA Science Mission Directorate [NNX08AR22G]
- NSF [AST-1238877]
- Natural Science Foundation of China [11390374, 11033008]
- Deutsche Forschungsgemeinschaft [HE1356/45-2]
- Netherlands Research School for Astronomy (NOVA)
- Elite Network of Bavaria
- Science and Technologies Council UK [ST/L000709/1]
- Queen's University Belfast's contribution to the PanSTARRS1 science consortium
- European Union FP7 Programme ERC [291222]
- NASA [NNG08FD60C]
- STFC [ST/M003515/1, ST/L000709/1, ST/M001970/1] Funding Source: UKRI
- Science and Technology Facilities Council [ST/M003515/1, ST/M001970/1, ST/L000709/1] Funding Source: researchfish
- Direct For Mathematical & Physical Scien
- Division Of Astronomical Sciences [1238877] Funding Source: National Science Foundation
Hypervelocity stars (HVSs) travel with velocities so high that they exceed the escape velocity of the Galaxy. Several acceleration mechanisms have been discussed. Only one HVS (US 708, HVS 2) is a compact helium star. Here we present a spectroscopic and kinematic analysis of US 708. Traveling with a velocity of similar to 1200 kilometers per second, it is the fastest unbound star in our Galaxy. In reconstructing its trajectory, the Galactic center becomes very unlikely as an origin, which is hardly consistent with the most favored ejection mechanism for the other HVSs. Furthermore, we detected that US 708 is a fast rotator. According to our binary evolution model, it was spun-up by tidal interaction in a close binary and is likely to be the ejected donor remnant of a thermonuclear supernova.
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