Semper simplicissimam, fundamentalem solutionem quaere. Si simpliciter explicare non potes, non intellexisti. (R. Feynman)
Astrophotography by GrandpaJunkrat - ----- V582 Cep
Cosmology from my armchair..............................
I do it metric .............................................................. Location:
bastion@protonmail.com The Netherlands
Bortle 7 - 9
Overview and Scientific Classification
V582 Cep is a young pre‑main‑sequence variable star located in the star‑forming region OB3. Its behavior and infrared properties clearly indicate the presence of a circumstellar disk, making it a classic Class II Young Stellar Object (YSO).
Key characteristics:
Optical variability caused by accretion fluctuations and variable extinction
Infrared excess from warm dust in the inner disk
Location within a cluster of stars younger than ~2 Myr
Light‑curve behavior similar to T Tauri–type variables
Scientific classification:
Gaia DR3 2217998150488879232 - 326.3681241759004, 66.00460739133746
Object type - Pre‑main‑sequence star / Orion variable (young, irregular variable)
YSO class - Class II YSO (T Tauri–like pre‑main‑sequence star)
Spectral type - K type
Region - OB3, Cepheus
Distance - 870 pc
Variability - Irregular, accretion‑driven variability typical of classical T Tauri stars, optical fluctuations from hot spots and variable accretion, mild to moderate amplitude
Environment - Embedded in a dusty, active star‑forming region with reflection nebulae, molecular gas, multiple Class I and Class II YSOs, ongoing accretion and disk evolution
Stellar Mass Estimate
The mass of V582 Cep can be inferred from:
Its optical brightness (R ~12.6), the distance to NGC 7129 (~1 kpc), typical mass–luminosity relations for Class II YSOs, comparison with similar objects in the same cluster
These constraints place V582 Cep in the range:
→ ~1.0–1.5 solar masses
This makes it a low‑mass YSO, consistent with T Tauri stars, though slightly on the higher end of that category.
Age Estimate
The stellar population of OB3 has an age distribution of:
0.5–2 Myr, with most Class II objects around ~1 Myr
Because V582 Cep:
still has a well‑defined circumstellar disk, shows active accretion signatures, and lacks the steep SED of a Class I protostar,
its age is best described as:
→ ~1 Myr (order of magnitude)
This places it firmly in the early pre‑main‑sequence phase, but no longer embedded.
Spectral Energy Distribution (SED) Reconstruction
The SED of V582 Cep follows the standard pattern of a Class II YSO:
Optical (Gaia / ground‑based)
Dominated by the stellar photosphere, strong variability due to accretion and dust occultation, no extreme emission lines typical of Herbig Ae/Be stars
Near‑Infrared (2MASS: J, H, K)
Clear infrared excess, emission from warm dust in the inner disk (T ~1000–1500 K)
Mid‑Infrared (WISE: W1–W4)
Strong disk emission, SED slope consistent with Class II disk geometry, no rising envelope component.
Far‑Infrared (Spitzer / IRAS)
Flattening flux, indicates absence of a protostellar envelope, confirms the Class II evolutionary stage
SED summary:
Photospheric emission + warm circumstellar disk, typical of a Class II YSO
The orbital reconstruction to his place of birth for V582 Cep
Vertical oscilation of V582 Cep
