標(biāo)題: Titlebook: CO: Twenty-Five Years of Millimeter-Wave Spectroscopy; Proceedings of the 1 William B. Latter,Simon J. E. Radford,John Bally Conference pro [打印本頁(yè)] 作者: 變成小松鼠 時(shí)間: 2025-3-21 16:20
書(shū)目名稱CO: Twenty-Five Years of Millimeter-Wave Spectroscopy影響因子(影響力)
書(shū)目名稱CO: Twenty-Five Years of Millimeter-Wave Spectroscopy影響因子(影響力)學(xué)科排名
書(shū)目名稱CO: Twenty-Five Years of Millimeter-Wave Spectroscopy網(wǎng)絡(luò)公開(kāi)度
書(shū)目名稱CO: Twenty-Five Years of Millimeter-Wave Spectroscopy網(wǎng)絡(luò)公開(kāi)度學(xué)科排名
書(shū)目名稱CO: Twenty-Five Years of Millimeter-Wave Spectroscopy被引頻次
書(shū)目名稱CO: Twenty-Five Years of Millimeter-Wave Spectroscopy被引頻次學(xué)科排名
書(shū)目名稱CO: Twenty-Five Years of Millimeter-Wave Spectroscopy年度引用
書(shū)目名稱CO: Twenty-Five Years of Millimeter-Wave Spectroscopy年度引用學(xué)科排名
書(shū)目名稱CO: Twenty-Five Years of Millimeter-Wave Spectroscopy讀者反饋
書(shū)目名稱CO: Twenty-Five Years of Millimeter-Wave Spectroscopy讀者反饋學(xué)科排名
作者: ARCHE 時(shí)間: 2025-3-21 22:55 作者: Alienated 時(shí)間: 2025-3-22 01:03 作者: Embolic-Stroke 時(shí)間: 2025-3-22 05:47 作者: 禍害隱伏 時(shí)間: 2025-3-22 12:33 作者: 出來(lái) 時(shí)間: 2025-3-22 14:57 作者: 出來(lái) 時(shí)間: 2025-3-22 18:26
A Molecular Worm in Scutumrvations have so far been confined mainly to several vertical strips across the plane covering a few degrees in Galactic longitude and 6°‐8° in Galactic latitude; details of this on-going survey are given in Dame & Thaddeus (1995).作者: 斜谷 時(shí)間: 2025-3-22 21:45
On the Fractal Structure of Molecular Cloudsmportant to study the power spectrum of observed cloud images. For HI clouds (Green 1993), the azimuthally averaged power spectra derived directly from interferometer observations are well characterized by a power law with a spectral index close to 2.8.作者: intercede 時(shí)間: 2025-3-23 03:28 作者: CRASS 時(shí)間: 2025-3-23 06:13
https://doi.org/10.1007/978-3-319-59957-1sed to determine the CR density and calibrate the CO line as a tracer of molecular mass. Dominant production mechanisms for γ rays of energies ～30 MeV-30 GeV are the decay of pions produced in collisions of CR protons with ambient matter and Bremsstrahlung scattering of CR electrons.作者: 隱藏 時(shí)間: 2025-3-23 13:16 作者: verdict 時(shí)間: 2025-3-23 16:48 作者: 言行自由 時(shí)間: 2025-3-23 21:35 作者: Yag-Capsulotomy 時(shí)間: 2025-3-24 00:44 作者: antenna 時(shí)間: 2025-3-24 04:21 作者: Parameter 時(shí)間: 2025-3-24 09:33
Narratives of Hurricane Katrina in Contextrmediate latitudes. I will also briefly describe work in progress on M31. It will be argued in conclusion that a complete Galactic CO survey at an angular resolution of 1′ is quite feasible with a dedicated multiple-feed telescope.作者: COW 時(shí)間: 2025-3-24 12:19
https://doi.org/10.1007/978-3-319-59957-1rvations have so far been confined mainly to several vertical strips across the plane covering a few degrees in Galactic longitude and 6°‐8° in Galactic latitude; details of this on-going survey are given in Dame & Thaddeus (1995).作者: Filibuster 時(shí)間: 2025-3-24 18:05
https://doi.org/10.1007/978-3-031-07773-9mportant to study the power spectrum of observed cloud images. For HI clouds (Green 1993), the azimuthally averaged power spectra derived directly from interferometer observations are well characterized by a power law with a spectral index close to 2.8.作者: 危機(jī) 時(shí)間: 2025-3-24 19:38 作者: Migratory 時(shí)間: 2025-3-25 00:28
Narratives of Hurricane Katrina in Contextefficient way for the atomic gas in the disk to lose angular momentum, or both, leading to measurable infall or inflow velocities. The truncation radius of CO is probably due to the recently identified stellar bar.作者: impale 時(shí)間: 2025-3-25 03:46 作者: 辯論 時(shí)間: 2025-3-25 09:52
Dubravka Zarkov,Marlies Glasiusonds to the Cepheus region while the second field contains the W3, W4, and W5 complex of HII regions. To date, 700,000 CO spectra have been collected. In this contribution, we present preliminary results from the first year of observations.作者: tariff 時(shí)間: 2025-3-25 13:27
CO in the Milky Wayefficient way for the atomic gas in the disk to lose angular momentum, or both, leading to measurable infall or inflow velocities. The truncation radius of CO is probably due to the recently identified stellar bar.作者: 結(jié)束 時(shí)間: 2025-3-25 16:14 作者: 特征 時(shí)間: 2025-3-25 23:39
FCRAO CO Survey of the Outer Galaxyonds to the Cepheus region while the second field contains the W3, W4, and W5 complex of HII regions. To date, 700,000 CO spectra have been collected. In this contribution, we present preliminary results from the first year of observations.作者: myalgia 時(shí)間: 2025-3-26 03:25
Present and Future CO Surveysveys. For several reasons, however, these have been done less systematically and less completely than the early 21 cm surveys; a great deal remains to be done. After a very brief general summary of what has been learned, I will emphasize the work now underway on the outer Galaxy and at high and inte作者: Nmda-Receptor 時(shí)間: 2025-3-26 07:22
CO in the Milky Wayes easier to understand the evolution of the disk of stars. The star formation rate per unit molecular gas mass is constant as a function of radius, and the H. depletion time turns out to be only a few percent of the Hubble time. This very short timescale requires that the atomic gas act as a reserv作者: Haphazard 時(shí)間: 2025-3-26 11:59 作者: Isometric 時(shí)間: 2025-3-26 13:20 作者: Ornithologist 時(shí)間: 2025-3-26 19:40
CO and the Multiphase ISMinterstellar medium. The trace ionization within the molecular gas is governed primarily by UV photoionization. Magnetic fields contribute a significantly larger fraction of the pressure in molecular clouds than in the diffuse interstellar medium. Observations suggest that the total Alfvén Mach numb作者: 向下 時(shí)間: 2025-3-26 22:04
The Ursa Major Molecular Cloudsentered at (.) ～ (138°,30°) and easily seen in IRAS 100 μm emission, is some 60 pc across and 150 pc distant (Meyerdierks et. al 1991). At 100 μm, the Ursa Major clouds appear in projection as “finger” (. ～ 140,. ～; 38) which “hangs down” towards the center of the loop and the plane of the Galaxy. D作者: GUILE 時(shí)間: 2025-3-27 02:47 作者: 珍奇 時(shí)間: 2025-3-27 05:27
The CO 2-1/1-0 Ratio solar neighborhood exhibit variations of the .=2?1/ .=l?0 intensity ratio from place to place in a cloud and from one cloud to another. This mainly reflects a variation of the hydrogen density near the ., where the opacity of the lines reaches ～ 1 at cloud surfaces. The ratio often exceeds unity at作者: 曲解 時(shí)間: 2025-3-27 10:44 作者: Project 時(shí)間: 2025-3-27 16:37
On the Fractal Structure of Molecular Cloudsects of star formation. Being generated predominantly by the turbulent internal cloud motion, the structure of molecular clouds is likely to be random to a large degree. As the information on the structural properties of random function is basically contained in its power spectrum, it is obviously i作者: grandiose 時(shí)間: 2025-3-27 21:21 作者: 親密 時(shí)間: 2025-3-28 00:40 作者: 偏離 時(shí)間: 2025-3-28 05:23 作者: 冷峻 時(shí)間: 2025-3-28 07:17
Narratives of Hurricane Katrina in Contextes easier to understand the evolution of the disk of stars. The star formation rate per unit molecular gas mass is constant as a function of radius, and the H. depletion time turns out to be only a few percent of the Hubble time. This very short timescale requires that the atomic gas act as a reserv作者: 破譯密碼 時(shí)間: 2025-3-28 14:02
https://doi.org/10.1007/978-3-319-59957-1a sensitivity per solid angle 3-10 times higher than previous CO surveys of the plane, and 16 times higher than the only previous extensive wide-latitude survey (Dame et al. 1987). Since a preliminary purpose of this survey is the study of molecular gas out of the plane in the inner Galaxy, the obse作者: Mosaic 時(shí)間: 2025-3-28 14:59
https://doi.org/10.1007/978-3-319-59957-1ry to study diffuse γ-ray emission from the interstellar medium (ISM). High-energy γ rays produced in cosmic-ray (CR) interactions in the ISM can be used to determine the CR density and calibrate the CO line as a tracer of molecular mass. Dominant production mechanisms for γ rays of energies ～30 MeV作者: dendrites 時(shí)間: 2025-3-28 20:18
Springer Series in Transitional Justiceinterstellar medium. The trace ionization within the molecular gas is governed primarily by UV photoionization. Magnetic fields contribute a significantly larger fraction of the pressure in molecular clouds than in the diffuse interstellar medium. Observations suggest that the total Alfvén Mach numb作者: reception 時(shí)間: 2025-3-29 02:43 作者: 安慰 時(shí)間: 2025-3-29 03:19
Dubravka Zarkov,Marlies Glasiusponent of the interstellar medium and to determine the relationship of this component to spiral arm features. When completed in Spring 1996, the CO Survey will cover 103° < .. < 145°, -3° < .. < 5°, and ?150 < V. < 50 km s. with angular sampling of 50″ and velocity resolution of 0.8 km s. . During t作者: 傳染 時(shí)間: 2025-3-29 07:25 作者: 喪失 時(shí)間: 2025-3-29 15:22 作者: GONG 時(shí)間: 2025-3-29 19:01
https://doi.org/10.1007/978-3-031-07773-9ects of star formation. Being generated predominantly by the turbulent internal cloud motion, the structure of molecular clouds is likely to be random to a large degree. As the information on the structural properties of random function is basically contained in its power spectrum, it is obviously i
