Akademik Veri Yönetim Sistemi
PHYSICA SCRIPTA, cilt.1, sa.1, ss.1-35, 2026 (SCI-Expanded, Scopus)
We present the first high-resolution near-infrared spectroscopic analysis of
the solar analog HD 115617 (61 Virginis), complemented by optical spectroscopy,
asteroseismology, and spectral energy distribution modeling. Using ESPRESSO and IGRINS
spectra with a newly calibrated NIR line list, we derived atmospheric parameters that revealed
notable differences between spectral regions: the optical analysis yielded Teff = 5500 ± 140
K, log g = 4.40 ± 0.16, and solar metallicity, whereas the NIR yielded Teff = 5750 ± 140
K. We tested this 250 K discrepancy using the independent line depth ratio (LDR) method for
both spectra. When applied to the optical lines, LDR confirmed the cooler scale (5553±73 K);
for the NIR lines, it provided an intermediate temperature (5636±15 K). Asteroseismic scaling
with TESS data yielded a radius of 0.98±0.09 R⊙, consistent with SED fitting and confirming
the star’s main-sequence solar-like status. However, the age estimates diverged between
methods, with optical and NIR analyses yielding ages of 10.97 and 8.04 Gyr, respectively.
Critically, a condensation temperature analysis revealed no significant trend, confirming the
star’s bulk solar-like composition and showing no chemical signature of planetary formation
processes. Kinematic diagnostics place HD 115617 in the thin Galactic disk, with a birth
radius of ∼ 5.7–8.0 kpc. Although the spectral differences may be linked to the star’s multiplanet system or debris disk, our analysis highlights the critical challenge of distinguishing
such effects from methodological systematics in multi-wavelength studies. Consequently,
we propose a systematic, homogeneous optical-NIR survey of solar-type stars to resolve this
ambiguity, which could ultimately inform novel indirect methods for characterizing stellar
environments.