標(biāo)題: Titlebook: Astrophysics in the Extreme Ultraviolet; Proceedings of Collo Stuart Bowyer (Professor in the Graduate School),R Conference proceedings 199 [打印本頁] 作者: EFFCT 時(shí)間: 2025-3-21 17:15
書目名稱Astrophysics in the Extreme Ultraviolet影響因子(影響力)
書目名稱Astrophysics in the Extreme Ultraviolet影響因子(影響力)學(xué)科排名
書目名稱Astrophysics in the Extreme Ultraviolet網(wǎng)絡(luò)公開度
書目名稱Astrophysics in the Extreme Ultraviolet網(wǎng)絡(luò)公開度學(xué)科排名
書目名稱Astrophysics in the Extreme Ultraviolet被引頻次
書目名稱Astrophysics in the Extreme Ultraviolet被引頻次學(xué)科排名
書目名稱Astrophysics in the Extreme Ultraviolet年度引用
書目名稱Astrophysics in the Extreme Ultraviolet年度引用學(xué)科排名
書目名稱Astrophysics in the Extreme Ultraviolet讀者反饋
書目名稱Astrophysics in the Extreme Ultraviolet讀者反饋學(xué)科排名
作者: strdulate 時(shí)間: 2025-3-21 20:49
Flex with Photoshop and Illustrator,exposure time, we have measured over 200 emission features with S/N ≥ 3.0 in the summed spectrum. We report here initial results from the analysis of this spectrum. We can now identify lines of Fe VIII and X-XIV, as well as a number of electron density and abundance diagnostic lines.作者: 運(yùn)動吧 時(shí)間: 2025-3-22 02:03 作者: 切掉 時(shí)間: 2025-3-22 04:39
Dissecting the EUV Spectrum of Capellaexposure time, we have measured over 200 emission features with S/N ≥ 3.0 in the summed spectrum. We report here initial results from the analysis of this spectrum. We can now identify lines of Fe VIII and X-XIV, as well as a number of electron density and abundance diagnostic lines.作者: Explicate 時(shí)間: 2025-3-22 12:27
Are Some Stellar Coronae Optically Thick?nse, hot flare plasmas. The electron densities of the 5–15 MK component are some three orders of magnitude higher than typical of the solar-like component around 2 MK; the volume filling factors of the hot components are therefore expected to be relatively small.作者: inspiration 時(shí)間: 2025-3-22 14:43 作者: induct 時(shí)間: 2025-3-22 20:13
Foundation Flash CS4 for DesignersI review some of the major achievements of the . extreme-ultraviolet all-sky survey, including the results of the recently completed 2RE source catalogue and associated study of temporal variability in EUV sources.作者: 性別 時(shí)間: 2025-3-22 22:58 作者: Deduct 時(shí)間: 2025-3-23 03:17
Introducing Flex and Flex Builder 3,“Yes, it will be a long time before people know what I know. How much of iron and other metal there is in the sun and the stars is easy to find out, but anything which exposes our swinishness is difficult, terribly difficult” (Tolstoy 1889).作者: 饒舌的人 時(shí)間: 2025-3-23 09:10 作者: curettage 時(shí)間: 2025-3-23 13:19
Results from the Second , Source CatalogWe present the results of the Second . Source Catalog, including all detections from the . all-sky survey, the . deep survey, and sources detected during dedicated instrument pointings. Where available, we furnish identifications of these objects and statistics with regard to type of stellar or extragalactic object.作者: 表否定 時(shí)間: 2025-3-23 15:27
The FIP Effect and Abundance Anomalies in Late-Type Stellar Coronae“Yes, it will be a long time before people know what I know. How much of iron and other metal there is in the sun and the stars is easy to find out, but anything which exposes our swinishness is difficult, terribly difficult” (Tolstoy 1889).作者: 惡意 時(shí)間: 2025-3-23 19:52 作者: 疼死我了 時(shí)間: 2025-3-23 22:50
https://doi.org/10.1007/978-1-4302-0481-7ource type as follows: cataclysmic variables 9, late-type (F-M) stars 18, the high-mass X-ray binary Her X-1, the eclipsing binaries Algol and V471 Tau, and the active galaxy Mkn 478. The most highly variable objects in the EUV band are cataclysmic variables. The survey was sensitive to timescales f作者: 的闡明 時(shí)間: 2025-3-24 04:24
Foundation Flash Cartoon Animation1995, to observe the sky area around the HZ 43 close to the north galactic pole. The wave bands (δλ ～ 10 ?) are provided at 130 and 170 ? by the multilayer coating on the reflectors of 20 cm in diameter and of 30 cm in focal length. The focal plane images are detected by CsI coated MCP’s. The observ作者: hankering 時(shí)間: 2025-3-24 07:09 作者: 致命 時(shí)間: 2025-3-24 14:40 作者: Commentary 時(shí)間: 2025-3-24 17:50
Foundation Flash Cartoon Animationr AGN in directions of low galactic absorption. It is found that the best-fit power-law photon indices of the X-ray spectra at 0.1-2.4 keV are anti-correlated with their galactic hydrogen columns. The indices for the 0.9-2.4 keV range do not show such a correlation, and are considerably smaller (i.e作者: Decline 時(shí)間: 2025-3-24 19:21
Custom Components and Library Packages,VII emission at 70 ?. The lines show significant broadening (FWHM 3800 km s.) placing the emitting region at the same distance as the inner broad-line region. A fit to a thermal plasma yields a temperature of 6 × 10. K. The line emission can be attributed to the warm absorbing material discovered be作者: 強(qiáng)所 時(shí)間: 2025-3-25 01:20 作者: 軟弱 時(shí)間: 2025-3-25 06:57 作者: 不確定 時(shí)間: 2025-3-25 08:26 作者: 跳脫衣舞的人 時(shí)間: 2025-3-25 13:02
Developing the Message Display Modulethan 10,000 s. The spectrum is characterized by several features between 80 and 100 ?. We compare the observed data with several models. We can rule out the possibility that the EUV emission is from a diffuse corona or intercloud medium. Models that assume the soft X-ray/EUV emission results from re作者: 講個(gè)故事逗他 時(shí)間: 2025-3-25 19:01 作者: Felicitous 時(shí)間: 2025-3-25 21:57 作者: Decline 時(shí)間: 2025-3-26 03:42
Flex with Photoshop and Illustrator, a continuous distribution of temperatures (～ 10. - 10. K). In addition to the strong He II A303.8, the spectra are dominated by emission lines of highly ionized iron. Strong lines of Fe IX, XV, XVI, and XVIII-XXIV are used to construct emission measure distributions for the individual pointings, wh作者: FEAT 時(shí)間: 2025-3-26 06:49 作者: ARK 時(shí)間: 2025-3-26 11:07
Flex Video Gallery with Drag-and-Drop,elatively weak component between 0.1 MK and 1 MK, (b) a dominant component somewhere between 2 MK and 10 MK, and (c) in all cases but one a component in the formal solution at temperatures exceeding ≈ 20 MK. Where this hot tail is not associated with a real hot component, it is a spurious result ref作者: Biguanides 時(shí)間: 2025-3-26 16:25
https://doi.org/10.1007/978-94-011-3988-5active galactic nuclei; astronomy; astrophysics; interstellar matter; neutron star; solar system; star; ste作者: 能得到 時(shí)間: 2025-3-26 17:19 作者: 哥哥噴涌而出 時(shí)間: 2025-3-26 23:32 作者: Microaneurysm 時(shí)間: 2025-3-27 02:32 作者: 使混合 時(shí)間: 2025-3-27 09:16 作者: Cardiac 時(shí)間: 2025-3-27 11:30 作者: 彈藥 時(shí)間: 2025-3-27 17:29 作者: ALLEY 時(shí)間: 2025-3-27 21:00
Discovery of Warm Gas in the Virgo Clustertended emission, were detected in the 0.065–0.248 keV band. A detailed comparison of these data with the . PSPC data of M87 revealed an excess flux at energies < 0.4 keV within the central 30′ radius which cannot be associated with the well-known cluster gas at X-ray temperatures (kT ≥ a few keV). I作者: definition 時(shí)間: 2025-3-28 00:29
EUV and Soft X-ray Evidence for Partially Ionized Gas in Active Galactic Nucleir AGN in directions of low galactic absorption. It is found that the best-fit power-law photon indices of the X-ray spectra at 0.1-2.4 keV are anti-correlated with their galactic hydrogen columns. The indices for the 0.9-2.4 keV range do not show such a correlation, and are considerably smaller (i.e作者: SLING 時(shí)間: 2025-3-28 03:13 作者: apiary 時(shí)間: 2025-3-28 08:16 作者: 小平面 時(shí)間: 2025-3-28 13:28 作者: 卡死偷電 時(shí)間: 2025-3-28 18:34 作者: 吵鬧 時(shí)間: 2025-3-28 21:04
Observations of the Seyfert Galaxy MRK 279than 10,000 s. The spectrum is characterized by several features between 80 and 100 ?. We compare the observed data with several models. We can rule out the possibility that the EUV emission is from a diffuse corona or intercloud medium. Models that assume the soft X-ray/EUV emission results from re作者: DEAWL 時(shí)間: 2025-3-29 00:40 作者: 草本植物 時(shí)間: 2025-3-29 05:31 作者: 眼界 時(shí)間: 2025-3-29 10:46 作者: 健壯 時(shí)間: 2025-3-29 14:47 作者: 艱苦地移動 時(shí)間: 2025-3-29 18:14 作者: 亞當(dāng)心理陰影 時(shí)間: 2025-3-29 20:35
s deemed to be the `unobservableultraviolet‘. Pioneering results from an EUV telescope on theApollo-Soyuz Mission in 1975 forcibly demonstrated that thisview was incorrect; but it required the all-sky surveys of the EnglishWide-Field Camera and the Extreme Ultraviolet Explorer to demonstratethe broa作者: NOMAD 時(shí)間: 2025-3-30 03:14
Making Flash Not Look Like Flash, objects, have already been identified, and spectroscopic measurements of several of them have yielded a number of surprises. However, more observations are clearly needed to confirm some of the reported spectral features and to validate their interpretation.作者: 激怒某人 時(shí)間: 2025-3-30 07:01
Custom Components and Library Packages, region. A fit to a thermal plasma yields a temperature of 6 × 10. K. The line emission can be attributed to the warm absorbing material discovered before from oxygen and iron absorption features, which appears to be an optically thin (for the Lyman continuum), highly ionized phase of the broad-line region.作者: 肌肉 時(shí)間: 2025-3-30 10:55
Custom Components and Library Packages,the EUV flux is, in fact, composed partly of line emission, we consider the implications if this is the result of emission from a collision-driven plasma at temperatures ? 10. K. In this context, we discuss some of the constraints imposed on the emission-line region by this observation.作者: BIPED 時(shí)間: 2025-3-30 16:17
Developing the Message Display Moduleut the possibility that the EUV emission is from a diffuse corona or intercloud medium. Models that assume the soft X-ray/EUV emission results from reprocessing in an optical BLR region are also inconsistent with the data. A collisional excitation model is consistent with the observations but requires a cloud density ≥ 10. cm..作者: 內(nèi)部 時(shí)間: 2025-3-30 17:35
Behind the Scenes II: MySQL and Data Storage are discussed. The importance of the geometry adopted when interpreting the emission measure distribution is stressed, since radial factors can lead to an . emission measure distribution gradient that is steeper than the value of 3/2 expected in plane parallel geometry.作者: 整潔漂亮 時(shí)間: 2025-3-30 23:32
Active Galactic Nuclei in the Extreme Ultraviolet objects, have already been identified, and spectroscopic measurements of several of them have yielded a number of surprises. However, more observations are clearly needed to confirm some of the reported spectral features and to validate their interpretation.作者: 使聲音降低 時(shí)間: 2025-3-31 04:36
Line Emission from Warm Material in NGC 5548 region. A fit to a thermal plasma yields a temperature of 6 × 10. K. The line emission can be attributed to the warm absorbing material discovered before from oxygen and iron absorption features, which appears to be an optically thin (for the Lyman continuum), highly ionized phase of the broad-line region.作者: CULP 時(shí)間: 2025-3-31 09:04 作者: 天空 時(shí)間: 2025-3-31 11:01
Observations of the Seyfert Galaxy MRK 279ut the possibility that the EUV emission is from a diffuse corona or intercloud medium. Models that assume the soft X-ray/EUV emission results from reprocessing in an optical BLR region are also inconsistent with the data. A collisional excitation model is consistent with the observations but requires a cloud density ≥ 10. cm..作者: 愛社交 時(shí)間: 2025-3-31 14:41
Spectra of Coronae and Flares are discussed. The importance of the geometry adopted when interpreting the emission measure distribution is stressed, since radial factors can lead to an . emission measure distribution gradient that is steeper than the value of 3/2 expected in plane parallel geometry.作者: 衰弱的心 時(shí)間: 2025-3-31 18:17
https://doi.org/10.1007/978-1-4302-0481-7is unclear. Both the temperature and spatial extent argue against cooling flow as the primary process responsible for its production. Other mechanisms, such as a galactic wind and heating by galaxy motions, must be considered.作者: 閑逛 時(shí)間: 2025-3-31 22:13
Discovery of Warm Gas in the Virgo Clusteris unclear. Both the temperature and spatial extent argue against cooling flow as the primary process responsible for its production. Other mechanisms, such as a galactic wind and heating by galaxy motions, must be considered.作者: Axillary 時(shí)間: 2025-4-1 02:38
Conference proceedings 1996eres and evolution, neutron stars,the Io torus, cataclysmic variable stars, active galactic nuclei, theinterstellar medium, winds and atmospheres of early type stars, andEUV plasma diagnostics. .Selected manuscripts from this meeting are provided in theseConference Proceedings.作者: Spongy-Bone 時(shí)間: 2025-4-1 09:14
