Titlebook: Cool Stars, Stellar Systems and the Sun; Proceedings of the F Michael Zeilik,David M. Gibson Conference proceedings 1986 Springer-Verlag Be

只看該作者 · 發(fā)表于 2025-3-21 16:49:32

書(shū)目名稱(chēng)Cool Stars, Stellar Systems and the Sun影響因子(影響力)

書(shū)目名稱(chēng)Cool Stars, Stellar Systems and the Sun影響因子(影響力)學(xué)科排名

書(shū)目名稱(chēng)Cool Stars, Stellar Systems and the Sun網(wǎng)絡(luò)公開(kāi)度

書(shū)目名稱(chēng)Cool Stars, Stellar Systems and the Sun網(wǎng)絡(luò)公開(kāi)度學(xué)科排名

書(shū)目名稱(chēng)Cool Stars, Stellar Systems and the Sun被引頻次

書(shū)目名稱(chēng)Cool Stars, Stellar Systems and the Sun被引頻次學(xué)科排名

書(shū)目名稱(chēng)Cool Stars, Stellar Systems and the Sun年度引用

書(shū)目名稱(chēng)Cool Stars, Stellar Systems and the Sun年度引用學(xué)科排名

書(shū)目名稱(chēng)Cool Stars, Stellar Systems and the Sun讀者反饋

書(shū)目名稱(chēng)Cool Stars, Stellar Systems and the Sun讀者反饋學(xué)科排名

只看該作者 · 發(fā)表于 2025-3-22 00:08:03

Correlation of the Mg II h & k flux versus rotational period in late-type stars,otational periods. It is shown that the relationship proposed by Hartmann et al for F to K stars does extend to the dMe stars, although there is more scatter. This is in part due to our inability to use the parameter representing the convective-overturn time.

只看該作者 · 發(fā)表于 2025-3-22 03:58:44

只看該作者 · 發(fā)表于 2025-3-22 07:58:07

只看該作者 · 發(fā)表于 2025-3-22 09:17:42

只看該作者 · 發(fā)表于 2025-3-22 16:44:08

只看該作者 · 發(fā)表于 2025-3-22 19:42:29

只看該作者 · 發(fā)表于 2025-3-23 00:40:16

Undesired Effects of Input Saturation,ctral types that, on the basis of current models, correspond to fully convective interiors. Hence, the results support a rotation-dependent distributed dynamo (or some variation thereof) as a viable model for the generation of magnetic flux in the very low mass stars. Future work should include v si

只看該作者 · 發(fā)表于 2025-3-23 04:48:03

Correlation of the Mg II h & k flux versus rotational period in late-type stars,otational periods. It is shown that the relationship proposed by Hartmann et al for F to K stars does extend to the dMe stars, although there is more scatter. This is in part due to our inability to use the parameter representing the convective-overturn time.

只看該作者 · 發(fā)表于 2025-3-23 07:03:04

Cool Stars, Stellar Systems and the Sun978-3-540-38731-2Series ISSN 0075-8450 Series E-ISSN 1616-6361

		自動(dòng)登錄	找回密碼
密碼			To register

關(guān)于派博傳思			派博傳思旗下網(wǎng)站			友情鏈接
派博傳思介紹	公司地理位置	論文服務(wù)流程	影響因子官網(wǎng)	吾愛(ài)論文網(wǎng)	大講堂	北京大學(xué)	Oxford Uni.	Harvard Uni.
發(fā)展歷史沿革	期刊點(diǎn)評(píng)	投稿經(jīng)驗(yàn)總結(jié)	SCIENCEGARD	IMPACTFACTOR	派博系數(shù)	清華大學(xué)	Yale Uni.	Stanford Uni.
\|Archiver\|手機(jī)版\|小黑屋\| 派博傳思國(guó)際 ( 京公網(wǎng)安備110108008328) GMT+8, 2026-1-21 15:29
Copyright © 2001-2015 派博傳思京公網(wǎng)安備110108008328 版權(quán)所有 All rights reserved