起草
发表于 2025-3-26 21:26:24
http://reply.papertrans.cn/88/8769/876860/876860_31.png
有恶臭
发表于 2025-3-27 03:19:28
Wolfgang Kohn,Riza Öztürkcess is also present in other nova-like objects and is specially important in old and slow novae (Callus et al, 1987) where the continuous ejection of mass produces dust shells which are strong emitters in the infrared.
雄伟
发表于 2025-3-27 07:07:54
http://reply.papertrans.cn/88/8769/876860/876860_33.png
transient-pain
发表于 2025-3-27 10:23:17
http://reply.papertrans.cn/88/8769/876860/876860_34.png
畸形
发表于 2025-3-27 14:06:48
http://reply.papertrans.cn/88/8769/876860/876860_35.png
奴才
发表于 2025-3-27 21:10:09
Wolfgang Kohn,Riza Öztürkcess is also present in other nova-like objects and is specially important in old and slow novae (Callus et al, 1987) where the continuous ejection of mass produces dust shells which are strong emitters in the infrared.
Rodent
发表于 2025-3-28 00:56:42
Wolfgang Kohn,Riza Öztürkcess is also present in other nova-like objects and is specially important in old and slow novae (Callus et al, 1987) where the continuous ejection of mass produces dust shells which are strong emitters in the infrared.
出汗
发表于 2025-3-28 03:32:47
Wolfgang Kohn,Riza Öztürkle novalike object. The spectrum of IRAS 06518 - 1041, which is shown in Figure 1, presents strong and broad hydrogen Balmer lines together with broad permitted lines of He and C. This spectrum also shows a much weaker narrow nebular component, with forbidden lines of and narrow Ha. The mean
vascular
发表于 2025-3-28 08:15:18
Wolfgang Kohn,Riza Öztürkle novalike object. The spectrum of IRAS 06518 - 1041, which is shown in Figure 1, presents strong and broad hydrogen Balmer lines together with broad permitted lines of He and C. This spectrum also shows a much weaker narrow nebular component, with forbidden lines of and narrow Ha. The mean
Adulate
发表于 2025-3-28 11:19:42
Wolfgang Kohn,Riza Öztürkle novalike object. The spectrum of IRAS 06518 - 1041, which is shown in Figure 1, presents strong and broad hydrogen Balmer lines together with broad permitted lines of He and C. This spectrum also shows a much weaker narrow nebular component, with forbidden lines of and narrow Ha. The mean