標(biāo)題: Titlebook: Dust-Gas Instabilities in Protoplanetary Disks; Toward Understanding Ryosuke Tominaga Book 2022 The Editor(s) (if applicable) and The Autho [打印本頁(yè)] 作者: 傳家寶 時(shí)間: 2025-3-21 16:54
書目名稱Dust-Gas Instabilities in Protoplanetary Disks影響因子(影響力)
書目名稱Dust-Gas Instabilities in Protoplanetary Disks影響因子(影響力)學(xué)科排名
書目名稱Dust-Gas Instabilities in Protoplanetary Disks網(wǎng)絡(luò)公開度
書目名稱Dust-Gas Instabilities in Protoplanetary Disks網(wǎng)絡(luò)公開度學(xué)科排名
書目名稱Dust-Gas Instabilities in Protoplanetary Disks被引頻次
書目名稱Dust-Gas Instabilities in Protoplanetary Disks被引頻次學(xué)科排名
書目名稱Dust-Gas Instabilities in Protoplanetary Disks年度引用
書目名稱Dust-Gas Instabilities in Protoplanetary Disks年度引用學(xué)科排名
書目名稱Dust-Gas Instabilities in Protoplanetary Disks讀者反饋
書目名稱Dust-Gas Instabilities in Protoplanetary Disks讀者反饋學(xué)科排名
作者: 織布機(jī) 時(shí)間: 2025-3-21 22:27 作者: 反抗者 時(shí)間: 2025-3-22 01:03 作者: 生意行為 時(shí)間: 2025-3-22 07:06 作者: 幻想 時(shí)間: 2025-3-22 09:59
Mariya Petrova,Seth J. Schwartzt radial drift. The contents of this chapter are based on our published paper: Tominaga et?al. (2019), ApJ, 881, 53, DOI: 10.3847/1538-4357/ab25ea. Figures and some texts are reproduced in this thesis with permission from American Astronomical Society (?AAS)作者: BRUNT 時(shí)間: 2025-3-22 15:45 作者: BRUNT 時(shí)間: 2025-3-22 17:38 作者: 解凍 時(shí)間: 2025-3-23 00:27
Introduction,ow in size through mutual sticking and form building blocks of planets called planetesimals. Further coalescence of planetesimals leads to formation of planets. However, it is known that there are some barriers against dust growth to planetesimals, and the formation process of planetesimals is still作者: 重畫只能放棄 時(shí)間: 2025-3-23 04:03 作者: 起來(lái)了 時(shí)間: 2025-3-23 06:12
Numerical Simulations of Secular Instabilities,erstand subsequent planetesimal formation. Because of the slow growth of the instability, one has to use numerical methods that are less diffusive and avoid numerical errors as much as possible. Motivated by this, we first formulate Lagrange-cell method for long-term hydrodynamic simulations. Our me作者: 案發(fā)地點(diǎn) 時(shí)間: 2025-3-23 12:55 作者: 聲明 時(shí)間: 2025-3-23 16:41
,Summary and?Future Prospects,here planetesimals form are not smooth profile as assumed in the classical standard theory but quite structured. Especially, dust rings and gaps have been frequently observed, which might be the key to explain dust growth toward planetesimals in protoplanetary disks. In this thesis, we investigate d作者: HUSH 時(shí)間: 2025-3-23 20:04 作者: insecticide 時(shí)間: 2025-3-24 01:25
Ryosuke TominagaHighlights new instability triggered by dust-gas friction and turbulent viscosity.Presents a new instability driven by dust coagulation in protoplanetary disks.Offers a planetesimal formation scenario作者: 提升 時(shí)間: 2025-3-24 02:23
Springer Theseshttp://image.papertrans.cn/e/image/283450.jpg作者: COM 時(shí)間: 2025-3-24 07:37 作者: Nmda-Receptor 時(shí)間: 2025-3-24 12:35 作者: terazosin 時(shí)間: 2025-3-24 18:45 作者: Preamble 時(shí)間: 2025-3-24 21:17 作者: 男學(xué)院 時(shí)間: 2025-3-25 01:05 作者: homeostasis 時(shí)間: 2025-3-25 05:39
Positive Youth Development in Chinaing secular gravitational instability. The previous dust-gas instabilities require super-solar metallicity and large dust grains whose dimensionless stopping time is 0.1–1. However, dust coagulation models have shown that dust growth proceeds in inside-out manner and the resulting radial drift cause作者: 可互換 時(shí)間: 2025-3-25 08:35
When Will a Repost Cascade Settle Down?here planetesimals form are not smooth profile as assumed in the classical standard theory but quite structured. Especially, dust rings and gaps have been frequently observed, which might be the key to explain dust growth toward planetesimals in protoplanetary disks. In this thesis, we investigate d作者: 性學(xué)院 時(shí)間: 2025-3-25 14:47 作者: Observe 時(shí)間: 2025-3-25 16:12
Carmen Buzea,Radosveta Dimitrova under debate. In this chapter, we briefly review disk formation from a molecular cloud core, basic dust dynamics in a disk, and recent high-resolution disk observations with Atacama Large Millimeter/submillimeter Array (ALMA) that provides hints to reveal planetesimal formation.作者: 上坡 時(shí)間: 2025-3-25 22:57 作者: 雪白 時(shí)間: 2025-3-26 04:06
Introduction, under debate. In this chapter, we briefly review disk formation from a molecular cloud core, basic dust dynamics in a disk, and recent high-resolution disk observations with Atacama Large Millimeter/submillimeter Array (ALMA) that provides hints to reveal planetesimal formation.作者: 膝蓋 時(shí)間: 2025-3-26 07:03
,Summary and?Future Prospects,ust-gas instabilities that have potential to explain dust ring formation and planetesimal formation based on linear analyses and numerical simulations. In this chapter, we summarize the studies presented in this thesis and describe future prospects.作者: 失眠癥 時(shí)間: 2025-3-26 10:08 作者: 肌肉 時(shí)間: 2025-3-26 14:05 作者: magenta 時(shí)間: 2025-3-26 17:28
9樓作者: 弓箭 時(shí)間: 2025-3-26 23:53
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9樓作者: 膠狀 時(shí)間: 2025-3-27 08:02
10樓作者: GLUT 時(shí)間: 2025-3-27 11:44
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