scholarly journals Propagating characteristics of mesospheric gravity waves observed by an OI 557.7 nm airglow all-sky camera at Mt. Bohyun (36.2°N, 128.9°E)

2021 ◽  
Author(s):  
Jun-Young Hwang ◽  
Young-Sook Lee ◽  
Yong Ha Kim ◽  
Hosik Kam ◽  
Young-Sil Kwak ◽  
...  

Abstract. We analyzed all-sky camera images observed at Mt. Bohyun observatory (36.2°N, 128.9°E) for the period of 2017–2019. The image data were acquired with a narrow band filter centered at 557.7 nm for the OI airglow emission at ~96 km altitude. The total of 150 wave events were identified in the images of 144 clear nights. The interquartile ranges of wavelength, phase speed, and periods of the identified waves are 20.5–35.5 km, 27.4–45.0 m/s and 10.8–13.7 min with the median values of 27.8 km, 36.3 m/s and 11.7 min, respectively. The summer and spring bias of propagation directions of northeast- and northward, respectively, can be interpreted as the effect of filtering by the prevailing winds in the lower atmosphere. In winter the subdominant northwestward waves may be observed due to nullified filtering effect by small northward background wind or secondary waves generated in the upper atmosphere. Intrinsic phase speeds and periods of the waves were also derived by using the wind data simultaneously observed by a nearly co-located meteor radar. The nature of vertical propagation was evaluated in each season. The majority of observed waves are found to be freely propagating, and thus can be attributed to wave sources in the lower atmosphere.

2019 ◽  
Vol 71 (1) ◽  
Author(s):  
Takeru Yamada ◽  
Takeshi Imamura ◽  
Tetsuya Fukuhara ◽  
Makoto Taguchi

AbstractThe reason for stationary gravity waves at Venus’ cloud top to appear mostly at low latitudes in the afternoon is not understood. Since a neutral layer exists in the lower part of the cloud layer, the waves should be affected by the neutral layer before reaching the cloud top. To what extent gravity waves can propagate vertically through the neutral layer has been unclear. To examine the possibility that the variation of the neutral layer thickness is responsible for the dependence of the gravity wave activity on the latitude and the local time, we investigated the sensitivity of the vertical propagation of gravity waves on the neutral layer thickness using a numerical model. The results showed that stationary gravity waves with zonal wavelengths longer than 1000 km can propagate to the cloud-top level without notable attenuation in the neutral layer with realistic thicknesses of 5–15 km. This suggests that the observed latitudinal and local time variation of the gravity wave activity should be attributed to processes below the cloud. An analytical approach also showed that gravity waves with horizontal wavelengths shorter than tens of kilometers would be strongly attenuated in the neutral layer; such waves should originate in the altitude region above the neutral layer.


2017 ◽  
Vol 9 (2) ◽  
pp. 1-8
Author(s):  
Chaolong Fang ◽  
Bo Dai ◽  
Qiao Xu ◽  
Qi Wang ◽  
Dawei Zhang

1998 ◽  
Vol 330 (2) ◽  
pp. 150-156 ◽  
Author(s):  
A. Andreev ◽  
Bl. Pantchev ◽  
P. Danesh ◽  
B. Zafirova ◽  
E. Karakoleva

1982 ◽  
Vol 72 (12) ◽  
pp. 1714 ◽  
Author(s):  
M. V. R. K. Murty ◽  
N. C. Das

1971 ◽  
Vol 83 ◽  
pp. 93 ◽  
Author(s):  
Torrence V. Johnson ◽  
Larry A. Lebofsky ◽  
Thomas B. McCord

2013 ◽  
Vol 33 (11) ◽  
pp. 1123003
Author(s):  
罗昕 Luo Xin ◽  
邹喜华 Zou Xihua ◽  
温坤华 Wen Kunhua ◽  
潘炜 Pan Wei ◽  
闫连山 Yan Lianshan ◽  
...  

2010 ◽  
Vol 22 (8) ◽  
pp. 1819-1822
Author(s):  
岳威 Yue Wei ◽  
洪冬梅 Hong Dongmei ◽  
刘国喜 Liu Guoxi ◽  
韩永昶 Han Yongchang ◽  
刘连泽 Liu Lianze ◽  
...  

1982 ◽  
Vol 99 ◽  
pp. 531-537
Author(s):  
Michael M. Shara ◽  
Anthony F. J. Moffat

A search to continuum magnitude B ∼ 21.5 (MB∼ −3) using a narrow band filter at λ4670å and a wide B-band filter has revealed 21 Wolf-Rayet star candidates in about half the giant Sb galaxy M31. Some weak-line WR stars, particularly WN subtypes, may have escaped detection. These numbers are compatible with the total number of luminous (i.e. massive) stars in M31. Eighteen of twenty confirmed candidate stars in M31 lie in the direction of 0B associations in the ring of prominent star formation 5–16 kpc from the center.


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