Semper simplicissimam, fundamentalem solutionem quaere. Si simpliciter explicare non potes, non intellexisti. (R. Feynman)
Astrophotography by GrandpaJunkrat - ----- HIP 107207
Cosmology from my armchair..............................
I do it metric .............................................................. Location:
bastion@protonmail.com The Netherlands
Bortle 7 - 9
Overview and Scientific Classification
HIP 107207, also known as BD+65 1636, is identified in SIMBAD as a young stellar object located in the region of NGC 7129, a well‑known site of recent star formation. The star is associated with infrared emission and appears in multiple infrared surveys, indicating the presence of circumstellar material. Its environment contains reflection nebulae and embedded protostars, consistent with an early evolutionary stage. HIP 107207 is therefore considered part of the young pre‑main‑sequence population in this active star‑forming complex.
Scientific classification
Catalog entries classify HIP 107207 as a young stellar object (YSO) and an infrared source. It appears in several major catalogs, including BD, 2MASS, Tycho‑2, and Gaia releases, confirming its identification across optical and infrared wavelengthsSIMBAD Astronomical Database. Its classification as a YSO suggests ongoing or recent accretion activity and the likely presence of a circumstellar disk, typical of stars still contracting toward the main sequence.
Stellar Mass Estimate
Because HIP 107207 is embedded in a star‑forming region and catalog data provide no direct mass measurement, its mass must be inferred from its classification as a young stellar object. YSOs in NGC 7129 typically span masses from roughly one to a few solar masses, depending on their evolutionary stage. Given its detection in optical and infrared surveys and its classification as a YSO rather than a deeply embedded protostar, HIP 107207 is likely an intermediate‑ or low‑mass pre‑main‑sequence star, plausibly in the range of one to two solar masses. This remains an estimate due to the absence of published spectroscopic constraints.
Age Estimate
The NGC 7129 star‑forming region hosts a population with characteristic ages of less than a few million years, and HIP 107207 is explicitly listed as a young stellar object within this environment. Its youth is supported by its infrared excess and association with active star‑formation tracers. A reasonable age estimate places HIP 107207 at approximately one to three million years, consistent with other pre‑main‑sequence stars in the same cluster.
Spectral Energy Distribution (SED) Reconstruction
The SED of HIP 107207 is expected to show a combination of photospheric emission at optical wavelengths and a significant infrared excess due to circumstellar dust, as indicated by its identification as an infrared source in 2MASS and other IR catalogs. The infrared excess suggests the presence of a warm disk or envelope, typical of YSOs in the Class II regime. Extinction from surrounding molecular material likely suppresses the optical flux, while the infrared portion of the SED rises due to thermal emission from dust. A reconstructed SED would therefore show a reddened stellar component transitioning into a strong near‑ and mid‑infrared excess characteristic of disk‑bearing young stars.
