Photoevaporative Dispersal of Protoplanetary Disks around Evolving Intermediate-mass Stars

被引：21

作者：

Kunitomo, Masanobu ^{[1
]}

Ida, Shigeru ^{[2
]}

Takeuchi, Taku ^{[3
]}

Panic, Olja ^{[4
]}

Miley, James M. ^{[4
,5
,6
]}

Suzuki, Takeru K. ^{[7
]}

机构：

[1] Kurume Univ, Sch Med, Dept Phys, 67 Asahimachi, Kurume, Fukuoka 8300011, Japan

[2] Tokyo Inst Technol, Earth Life Sci Inst, Meguro Ku, 2-12-1 Ookayama, Tokyo 1528551, Japan

[3] Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, 2-12-1 Ookayama, Tokyo 1528550, Japan

[4] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England

[5] Joint ALMA Observ, Alonso Cordova 3107, Santiago, Chile

[6] Natl Astron Observ Japan, Alonso Cordova 3788,61B Vitacura, Santiago, Chile

[7] Univ Tokyo, Sch Arts & Sci, Meguro Ku, 3-8-1 Komaba, Tokyo 1538902, Japan

来源：

ASTROPHYSICAL JOURNAL | 2021年 / 909卷 / 02期

关键词：

Protoplanetary disks; Stellar accretion disks; Pre-main sequence stars; Stellar evolution; X-RAY-EMISSION; HERBIG AE/BE STARS; RADIATION HYDRODYNAMICS SIMULATIONS; GAS GIANT PLANETS; T-TAURI STARS; MAGNETOROTATIONAL INSTABILITY; CIRCUMSTELLAR DISKS; FAR-ULTRAVIOLET; EXTREME-ULTRAVIOLET; GLOBAL SIMULATIONS;

D O I：

10.3847/1538-4357/abdb2a

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We aim to understand the effect of stellar evolution on the evolution of protoplanetary disks. We focus in particular on the disk evolution around intermediate-mass (IM) stars, which evolve more rapidly than low-mass ones. We numerically solve the long-term evolution of disks around 0.5-5 M-circle dot stars considering viscous accretion and photoevaporation (PE) driven by stellar far-ultraviolet (FUV), extreme-ultraviolet (EUV), and X-ray emission. We also take stellar evolution into account and consider the time evolution of the PE rate. We find that the FUV, EUV, and X-ray luminosities of IM stars evolve by orders of magnitude within a few million years, along with the time evolution of stellar structure, stellar effective temperature, or accretion rate. Therefore, the PE rate also evolves with time by orders of magnitude, and we conclude that stellar evolution is crucial for the disk evolution around IM stars.

引用

页数：16

共 50 条

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