Semper simplicissimam, fundamentalem solutionem quaere. Si simpliciter explicare non potes, non intellexisti. (R. Feynman)
Astrophotography by GrandpaJunkrat - ----- TIC 322312503
Cosmology from my armchair..............................
I do it metric .............................................................. Location:
bastion@protonmail.com The Netherlands
Bortle 7 - 9
Overview and Scientific Classification
TIC 322312572, identified as ZTF J214242.82+661228.2, is classified as an eclipsing binary system located at a distance of roughly 900 parsecs based on its Gaia parallax. Its additional identifications as a near‑infrared and infrared source indicate the presence of warm stellar components or mild circumstellar material, while its possible classification as a young stellar object suggests that the system may lie within or near an active star‑forming environment. The combination of optical variability and infrared brightness makes it a notable system for studying binary evolution and early stellar development.
Scientific classification
The primary classification of the object as an eclipsing binary (EB*) indicates that its variability is caused by periodic mutual occultations of two orbiting stars. The Gaia classification confirms it as a stellar point source, while the tentative YSO designation suggests that at least one component may be relatively young. Its infrared detections in 2MASS and the SVS76 catalog imply that the system contains stars with moderate reddening or weak infrared excess. Together, these properties describe a compact binary system with components that may still be evolving toward the main sequence.
Stellar Mass Estimate
Because TIC 322312572 is an eclipsing binary, its total mass depends on the properties of both stellar components. In the absence of a published orbital solution, the mass must be inferred from its brightness and colors. The Gaia G magnitude of about 13.97 and the near‑infrared magnitudes (J ≈ 11.67, H ≈ 11.04, K ≈ 10.82) suggest that the system is composed of two low‑mass or solar‑type stars. A reasonable estimate places each component in the range of 0.7 to 1.1 solar masses, depending on their temperature contrast and luminosity ratio. The combined system mass is therefore likely between 1.4 and 2.2 solar masses.
Age Estimate
The possible classification as a young stellar object suggests that the system may be relatively young, but the evidence is not definitive. If the YSO flag reflects a true association with a star‑forming region, the system could be only a few million years old. However, if the classification is uncertain, as indicated by the Y*? tag, the system may instead be a mature field eclipsing binary. Given the lack of strong infrared excess or emission‑line activity, a conservative interpretation places the age anywhere from several hundred million years to a few billion years unless additional youth indicators are confirmed.
Spectral Energy Distribution (SED) Reconstruction
The photometric data show a smooth decline from the optical into the infrared, with no strong excess at longer wavelengths. The Gaia G magnitude near 14 and the near‑infrared magnitudes around 11 indicate a system dominated by stellar photospheric emission. The SED would therefore display two blended stellar components producing a combined spectrum typical of late‑type or solar‑type stars. The absence of a significant infrared excess suggests that the system lacks a substantial circumstellar disk, consistent with a relatively evolved eclipsing binary rather than a deeply embedded young system.
