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36 - Social play: history of the studies at Mahale and a new perspective
from Part VII - Social behavior
- By Masaki Shimada, Takahisa Matsusaka, Hitoshige Hayaki
Edited by Michio Nakamura, Kyoto University, Japan, Kazuhiko Hosaka, Noriko Itoh, Kyoto University, Japan, Koichiro Zamma
Book:

Mahale Chimpanzees

Published online:

05 September 2015

Print publication:

10 September 2015, pp 496-509
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40 - Diversity of play
from Part VIII - Behavioral diversity
- By Takahisa Matsusaka, Masaki Shimada, Michio Nakamura
Edited by Michio Nakamura, Kyoto University, Japan, Kazuhiko Hosaka, Noriko Itoh, Kyoto University, Japan, Koichiro Zamma
Book:

Mahale Chimpanzees

Published online:

05 September 2015

Print publication:

10 September 2015, pp 544-555
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14 - Socialobject play among juvenile Japanese macaques: Comparison between the provisioned Arashiyama-Kyoto troop and the non-provisioned Kinkazan troop
from Part III - Cultural behaviour, social interactions and ecology
- By Masaki Shimada
Edited by Jean-Baptiste Leca, University of Lethbridge, Alberta, Michael A. Huffman, Kyoto University, Japan, Paul L. Vasey, University of Lethbridge, Alberta
Book:

The Monkeys of Stormy Mountain

Published online:

05 March 2012

Print publication:

19 January 2012, pp 258-282
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Radiatively driven winds of OB stars
Michihiro R. Shimada, Masaki Ito, Ryuko Hirata, Toshihiro Horaguchi
Journal:

Symposium - International Astronomical Union / Volume 162 / 1994

Published online by Cambridge University Press:

26 May 2016, pp. 487-489

Print publication:

1994
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We newly calculated the line radiative force with 520,000 atomic lines, which is twice as many as those of Abbott (1982), for OB supergiants. Our results are as follows. (1) The mass loss rates for O stars with Teff = 50,000K are seven times as large as Abbott's (1982) because of contribution from Fe iv lines. (2) Contribution from many weak lines increases the mass loss rates and decreases the wind velocities of OB stars within a temperature range of 10,000K ≤ Teff ≤ 30,000K. This result is qualitatively in accordance with the results from the recent observations of O stars. (3) The mass loss rates of OB stars depend on metallicity with Ṁ ∼ Z.

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