The Red Supergiant Progenitor of Type II Supernova 2024ggi
arxiv(2024)
摘要
We present a detailed analysis of the progenitor and its local environment
for the recently discovered type II supernova (SN) 2024ggi at a distance of
about 6.7 Mpc, by utilizing the pre-explosion images from the Hubble Space
Telescope (HST) and Spitzer Space Telescope. The progenitor is
identified as a red, bright variable star, with absolute F814W-band
magnitudes being -6.2 mag in 1995 to -7.2 mag in 2003, respectively,
consistent with that of a normal red supergiant (RSG) star. Combining with the
historical mid-infrared light curves, a pulsational period of about 379 days
can be inferred for the progenitor star. Fitting its spectral energy
distribution with stellar spectral models yields the stellar parameters of
temperature, radius and bolometric luminosity as T_*=3290_-27^+19 K,
R_*=887_-51^+60 R_⊙, and
log(L/L_⊙)=4.92_-0.04^+0.05, respectively. The above parameters
indicate that the progenitor of SN 2024ggi is consistent with the stellar
evolutionary track of a solar-metallicity massive star with an initial mass of
13_-1^+1 M_⊙. Moreover, our analysis indicates a relatively low
mass loss rate (i.e., < 3×10^-6 M_⊙ yr^-1) for the
progenitor compared to that inferred from the flashed spectra and X-ray
detection (i.e., 10^-2-10^-5 M_⊙ yr^-1), implying a
significant enhancement in mass loss within a few years prior to the explosion.
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