Semper simplicissimam, fundamentalem solutionem quaere. Si simpliciter explicare non potes, non intellexisti. (R. Feynman)
Astrophotography by GrandpaJunkrat - ----- IfAHA 777
Cosmology from my armchair..............................
I do it metric .............................................................. Location:
bastion@protonmail.com The Netherlands
Bortle 7 - 9
Overview and Scientific Classification
IfAHA 777 (TIC 322312950) is classified in SIMBAD as an Orion Variable, a group of young, irregularly varying pre‑main‑sequence stars typically associated with active star‑forming regions. Its additional classifications—young stellar object, emission‑line star, X‑ray source, and near‑infrared source—indicate a system with ongoing magnetic activity, circumstellar material, and variability driven by accretion or dust obscuration. The star is relatively faint in the optical (V ≈ 15.5) but significantly brighter in the near‑infrared, consistent with a young object still embedded in or surrounded by warm dust.
Scientific classification
The combination of object types assigned in SIMBAD places IfAHA 777 firmly within the family of low‑mass pre‑main‑sequence stars. Its designation as an Orion Variable (Or) and Young Stellar Object (YO) suggests a T Tauri–like nature, while the presence of emission lines (Em*) and X‑ray activity points to strong chromospheric and accretion‑related processes. The infrared brightness detected by 2MASS further supports the presence of a circumstellar disk or envelope. Together, these characteristics identify IfAHA 777 as an actively evolving, magnetically active young star.
Stellar Mass Estimate
With a Gaia parallax of roughly 1.00 mas, IfAHA 777 lies at a distance of about 1 kpc, typical for young stars in distant star‑forming complexes. Its optical faintness combined with strong infrared emission suggests a low‑mass pre‑main‑sequence star, likely in the range of 0.5 to 1.0 solar masses. This estimate is consistent with its classification as an Orion Variable and with the typical masses of T Tauri stars exhibiting similar photometric and spectroscopic properties.
Age Estimate
As an Orion Variable and young stellar object, IfAHA 777 is expected to be extremely young, with an age of only a few million years. The presence of emission lines, irregular variability, and infrared excess all point to a star that has not yet reached the main sequence and is still interacting with its circumstellar environment. Such stars typically fall within the 1–5 Myr age range, depending on their accretion history and disk evolution.
Spectral Energy Distribution (SED) Reconstruction
The available photometry shows a steep rise from the optical (V ≈ 15.5, G ≈ 14.7) into the near‑infrared (J ≈ 12.1, H ≈ 11.3, K ≈ 11.0), indicating significant reddening and thermal emission from circumstellar dust. This SED morphology is characteristic of young, disk‑bearing stars where the stellar photosphere is partially obscured by dust while the disk contributes strongly at longer wavelengths. A reconstructed SED would therefore show a heavily reddened stellar component in the optical, transitioning into a pronounced infrared excess consistent with a Class II–type pre‑main‑sequence object.
