HAZMAT. V. The ultraviolet and X-ray evolution of K stars

Tyler Richey-Yowell, Evgenya L. Shkolnik, Adam C. Schneider, Ella Osby, Travis Barman, Victoria S. Meadows

Research output: Contribution to journalArticlepeer-review


Knowing the high-energy radiation environment of a star over a planet’s formation and evolutionary period is critical in determining if that planet is potentially habitable and if any biosignatures could be detected, as UV radiation can severely change or destroy a planet’s atmosphere. Current efforts for finding a potentially habitable planet are focused on M stars, yet K stars may offer more habitable conditions due to decreased stellar activity and more distant and wider habitable zones (HZ). While M star activity evolution has been observed photometrically and spectroscopically, there has been no dedicated investigation of K-star UV evolution. We present the first comprehensive study of the near-UV, far-UV, and X-ray evolution of K stars. We used members of young moving groups and clusters ranging in age from 10 – 625 Myr combined with field stars and their archived GALEX UV and ROSAT X-ray data to determine how the UV and X-ray radiation evolve. We find that the UV and X-ray flux incident on a HZ planet is 5 - 50 times lower than that of HZ planets around early-M stars and 50 - 1000 times lower than those around late-M stars, due to both an intrinsic decrease in K dwarf stellar activity occurring earlier than for M dwarfs and the more distant location of the K dwarf HZ.

Original languageEnglish (US)
JournalUnknown Journal
StatePublished - Jan 2 2019


  • Stars: evolution
  • Stars: low-mass

ASJC Scopus subject areas

  • General

Fingerprint Dive into the research topics of 'HAZMAT. V. The ultraviolet and X-ray evolution of K stars'. Together they form a unique fingerprint.

Cite this