Semper simplicissimam, fundamentalem solutionem quaere. Si simpliciter explicare non potes, non intellexisti. (R. Feynman)
Astrophotography by GrandpaJunkrat - ----- V350 Cep
Cosmology from my armchair..............................
I do it metric .............................................................. Location:
bastion@protonmail.com The Netherlands
Bortle 7 - 9
Birthplace (Galactic coordinates, 1σ uncertainties):
l_birth = 105.740 ± 0.090 deg
b_birth = 10.775 ± 0.254 deg
d_birth = 872.8 ± 22.7 pc
π= 1.1461 [0.0282] mas , Proper motions mas/yr : -1.581 -3.654 [0.033 0.031 90]
, vr=… km/s?
Overview and Scientific Classification
V350 Cep is a young, eruptive pre‑main‑sequence star located in the star‑forming region OB3 in Cepheus. It is classified in SIMBAD as an Orion variable (Or\)*, a broad category that includes young, irregularly variable stars with active accretion.
It is identified as:
Class I protostar, strong infrared excess, near‑infrared excess present, high star‑formation probability, spectral type M2, disk‑bearing YSO (IR‑excess).
This combination indicates a young stellar object still surrounded by a substantial circumstellar disk and possibly a remnant envelope, with ongoing accretion activity.
Scientific classification:
Object type - Pre‑main‑sequence star / Orion variable
YSO class - Class I (protostar)
Spectral type - M2
Region - OB3, Cepheus
Distance - ~872 pc (Gaia parallax 1.1461 mas)
Variability - Eruptive, irregular, accretion‑driven
Environment - Embedded in a dusty, active star‑forming region
V350 Cep shows characteristics reminiscent of FUor‑like or EXor‑like eruptive behavior, although it does not fit cleanly into either category.
Stellar Mass Estimate
For a Class I M2‑type pre‑main‑sequence star, the mass is typically 0.4–0.6 solar masses. Given its luminosity inferred from strong IR excess, its early evolutionary stage, and its location in a young cluster, a reasonable estimate is:
This places V350 Cep in the low‑mass T Tauri regime, consistent with its spectral type and photometric behavior.
Age Estimate
Class I objects represent one of the earliest observable phases of low‑mass star formation.
Typical ages:
Class 0: < 0.1 Myr
Class I: ~0.1–0.5 Myr
Class II: ~1–3 Myr
Class III: ~5–10 Myr
Given its strong IR excess,, its NIR excess,, its eruptive variability, and its embedded environment, the most consistent estimate is:
This makes V350 Cep a very young protostellar object, still in the process of clearing its envelope and building its final mass.
Spectral Energy Distribution (SED) Reconstruction
Mid‑Infrared (WISE) Extremely strong IR excess:
W1–W2 ≈ 1.72
W2–W3 ≈ 3.97
W3–W4 ≈ 2.62
These colors place V350 Cep firmly in the Class I protostar region of WISE color–color diagrams, emission dominated by warm dust in the disk and inner envelope
Optical (Gaia, PS1)
Faint and reddened due to extinction
Gaia BP–RP ≈ 2.10 → consistent with an M‑type star
Strong variability in the optical bands
The SED shape is consistent with:
A central M‑type protostar, surrounded by a massive, optically thick disk, plus a remnant infalling envelope, with active accretion heating the inner disk.
This is exactly what you expect for a Class I eruptive YSO.
The orbital reconstruction to his place of birth for V350 Cep
Vertical oscilation of V350 Cep
