Cepheus Flare
A giant molecular cloud complex in Cepheus.
The Cepheus Flare is an Orion-like complex of giant molecular clouds in the constellation of Cepheus, centered around the star β Cephei. It lies roughly 300-450 parsecs from Earth and about 100 parsecs above the galactic plane, containing 2 solar masses of neutral hydrogen. The complex serves as a unique laboratory for studying sequential star formation due to its abundance of star-forming regions, dark nebulas, supernova remnants, and young stellar objects.
Quick Facts
- Constellation
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Contents
The Cepheus Flare is packed with dense dark nebulas and supernova remnants, alongside eight major cloud complexes and 208 identified dark clouds. Notable among these are LDN 1147, LDN 1148, LDN 1152, LDN 1155, LDN 1157, LBN 468, and Barnard 175. Star formation is widespread, producing Herbig-Haro objects and bright nebulosity around newborn stars. Shock fronts from this activity likely explain the wide range of velocities seen in the region. The cloud’s structure is intricate, featuring molecular filaments, low-density cavities, dense gas pockets, and expanding shells. An infrared loop called GIRL G109+10 helps trigger star formation here. While no high-mass stars are forming, the flare hosts several low-mass star-forming centers. The presence of five A-type and B-type stars in the Cepheus R2 association suggests intermediate-mass star formation happened not long ago. Other stars in the complex include SAO 19953, HD 212826, HD 216486, BD +69°1231, CV Cepheus, and BO Cepheus. Spatially linked to the flare is ASCC 127, a young moving group with roughly 3,179 members that appears to have carved out shells within the Cepheus Flare.
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