Intelligent Simulation and Optimization of Axial Flow Fan Based on CFD

zhang, shengli; sun, yupei; he, long; wang, changhao

doi:10.21203/rs.3.rs-2601774/v1

Cited by 1 publication

(1 citation statement)

References 17 publications

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“…world, and both professional and amateur astronomers reported their early observations of photometry (e.g., Silva 2023a; Vannini & Julio 2023a;Kendurkar & Balam 2023b;Silva 2023b;Vannini & Julio 2023b;Kendurkar & Balam 2023cBrothers et al 2023;Chen et al 2023;Daglas 2023;D'Avanzo et al 2023;Desrosiers et al 2023;Fowler et al 2023;González-Carballo et al 2023;Koltenbah 2023;Li et al 2023;Maund et al 2023;Mayya et al 2023;Pessev et al 2023;Sgro et al 2023;Singh et al 2023;Vannini 2023;Villafane et al 2023;Zimmerman et al 2024) and spectroscopy (e.g., BenZvi et al 2023aLundquist et al 2023;Stritzinger et al 2023;Zhang et al 2023;Zimmerman et al 2024) of this object. SN 2023ixf was classified as a Type II SN ) and showed a strong blue continuum and prominent optical flash-ionization features (H, He, N, and C) in its early-phase spectrum, all indicative of the presence of circumstellar medium (CSM).…”

Section: Introductionmentioning

confidence: 99%

Multiband Simultaneous Photometry of Type II SN 2023ixf with Mephisto and the Twin 50 cm Telescopes

Yang,

Liu,

Pan

et al. 2024

ApJ

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SN 2023ixf, recently reported in the nearby galaxy M101 at a distance of 6.85 Mpc, was one of the closest and brightest core-collapse supernovae in the last decade. In this work, we present multiwavelength photometric observation of SN 2023ixf with the Multi-channel Photometric Survey Telescope (Mephisto) in the uvgr bands and with the twin 50 cm telescopes in the griz bands. We find that the bolometric luminosity reached the maximum value of 3 × 1043 erg s−1 at 3.9 days after the explosion and fully settled onto the radioactive tail at ∼90 days. The effective temperature decreased from 3.2 × 104 K at the first observation and approached a constant of ∼(3000–4000) K after the first 2 months. The evolution of the photospheric radius is consistent with a homologous expansion with a velocity of 8700 km s−1 in the first 2 months, and it shrunk subsequently. Based on the radioactive tail, the initial nickel mass is about M Ni ∼ 0.098 M ⊙. The explosion energy and the ejecta mass are estimated to be E ≃ (1.0–5.7) × 1051 erg and M ej ≃ (3.8–16) M ⊙, respectively. The peak bolometric luminosity is proposed to be contributed by the interaction between the ejecta and the circumstellar medium (CSM). We find a shocked CSM mass of M CSM ∼ 0.013 M ⊙, a CSM density of ρ CSM ∼ 2.5 × 10−13 g cm−3, and a mass-loss rate of the progenitor of M ̇ ∼ 0.022 M ⊙ yr − 1 .

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