GoKawiilThis work was supported by JSPS KAKENHI grant nos. JP22H00158, JP22H01268, JP22K03624, JP23H04899, JP21K13963, JP24K00638, JP24K17105, JP21K13958, JP21H01095, JP23K20850, JP24H00253, JP21K03615, JP24K00677, JP20K14491, JP23H00151, JP19K21884, JP20H01947, JP20KK0071, JP23K20239, JP24K00672, JP24K17104, JP24K17093, JP20K04009, JP21H04493, JP20H01946, JP23K13154, JP19K14762, JP20H05857 and JP23K03459 and NASA grant nos. 80NSSC23K0646, 80NSSC20K0733, 80NSSC18K0978, 80NSSC20K0883, 80NSSC20K0737, 80NSSC24K0678, 80NSSC18K1684 and 80NNSC22K1922. L. Corrales acknowledges support from NSF award no. 2205918. C. Done acknowledges support from STFC through grant no. ST/T000244/1. L. Gallo acknowledges financial support from the Canadian Space Agency grant no. 18XARMSTMA. M. Sawada acknowledges support from the RIKEN Pioneering Project Evolution of Matter in the Universe (r-EMU) and the Rikkyo University Special Fund for Research (Rikkyo SFR). A. Tanimoto and the present research are supported, in part, by the Kagoshima University postdoctoral research program (KU-DREAM). S. Yamada acknowledges support by the RIKEN SPDR Program. I. Zhuravleva acknowledges partial support from the Alfred P. Sloan Foundation through the Sloan Research Fellowship. This material is based on the work supported by NASA under award no. 80GSFC24M0006. Part of this work was performed under the auspices of the US Department of Energy by Lawrence Livermore National Laboratory under contract no. DE-AC52-07NA27344. This work was supported by the JSPS Core-to-Core Program, JPJSCCA20220002. The material is based on the work supported by the Strategic Research Center of Saitama University. This research has made use of data obtained from the Chandra Data Archive provided by the Chandra X-ray Center (CXC). This research has made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. This research has made use of data from the NASA/ESA Hubble Space Telescope obtained from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, under NASA contract no. NAS 5-26555.
A fast starburst wind consumes most of the energy from supernovae
Why This Matters
This study reveals that rapid starburst winds can significantly consume the energy produced by supernovae, impacting galaxy evolution and feedback processes. Understanding these energetic interactions is crucial for advancing models of galaxy formation and the lifecycle of cosmic matter, which benefits both the tech industry involved in astrophysical research and consumers interested in space science advancements.
Key Takeaways
- Starburst winds can consume most of the energy from supernovae.
- This process influences galaxy evolution and feedback mechanisms.
- The findings enhance our understanding of cosmic matter cycles and astrophysical phenomena.
Get alerts for these topics