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| Photochromic pigments change their "colour" ( | spectral absorbance properties) upon light absorption. |
| spectral absorption maxima (in solution) | |
| The Fraunhofer lines are typical | spectral absorption lines. |
| Spectral acceleration (SA) is a unit measured in g (th | |
| d on a 2% probability of exceeding 0.2 second | spectral acceleration at 5 Hz in 50 years |
| Spectral acceleration, with a value related to the nat | |
| e seismic hazard maps are also produced using | spectral acceleration. |
| ate of the center of the peak, thus improving | spectral accuracy. |
| For example in | spectral analysis the expected peak shape is often kno |
| and synthesis techniques, including real time | spectral analysis and additive resynthesis, audio morp |
| rospectrophotometers used for non-destructive | spectral analysis and imaging of microscopic sampling |
| observatory is particularly well situated for | spectral analysis in astronomy, which requires a clear |
| analysis, then the method is called Gradient | spectral analysis (GSA), usually applied to short time |
| al operations such as electronic filters, for | spectral analysis and for synchronized display of data |
| However, in 2005, an extensive mass | spectral analysis showed that the actual structure is |
| Spectral analysis of the least volatile fraction revea | |
| the measurements of atmospheric electricity, | spectral analysis of rare-earth elements, wave guide t |
| For the | spectral analysis technique, see Least-squares spectra |
| Spectral analysis has shown traces of ice. | |
| Maximum entropy | spectral analysis (MaxEnt spectral analysis) is a meth |
| Spectral analysis and its applications (with D. G. Wat | |
| Detailed X-ray | spectral analysis has been performed on 123 X-ray sour |
| The multitaper | spectral analysis is a powerful nonparametric method t |
| Spectral analysis of Egeria shows it to be unusually h | |
| Advanced systems also perform | spectral analysis, ischemic burden evaluation, graph o |
| ach height in registers or channels for later | spectral analysis. |
| Model 1 suffers from the fact that the | spectral and temporal characteristics strongly resembl |
| ured work from artists such as Total Eclipse, | Spectral, and Voodoo People. |
| 18 Scorpii is a main sequence star of | spectral and luminosity type G2 Va. |
| , comprising Alnitak Aa (a blue supergiant of | spectral and luminosity type O9.7 Ibe, with an absolut |
| serial, atonal, microtonal, polymodal, | spectral and others, however his style has emerged int |
| Spectral and harmonic response | |
| d (sensor calibration, orbital drift, limited | spectral and directional sampling, etc.). |
| Each | spectral appearance precedes a tragic event on the rai |
| nds her ground against General Hadias and the | Spectral army in Australia, and the mighty Great Mazin |
| ital alongside other similarly dressed men, a | spectral army clutching briefcases and silently marchi |
| Casting Eternal Fires Volume 1 ( | Spectral Arts Productions, 2002) |
| Developed by | Spectral Associates in 1981, the game lulls players in |
| Spectral attenuation of fiber optics | |
| Bathochromic shift is a change of | spectral band position in the absorption, reflectance, |
| HDC (Hybrid Digital Coding) with SBR ( | spectral band replication) is a proprietary lossy audi |
| The instruments capture data in 36 | spectral bands ranging in wavelength from 0.4 µm to 14 |
| m resolution in two visible and two infra-red | spectral bands over two 100km swathes; "Visible and Th |
| HyMap data has 126 | spectral bands spanning the wavelengh interval 0.45-2. |
| ging Self Scanner (LISS-4) operating in three | spectral bands in the visible and Near Infrared Region |
| ring the 2009 and 2010 seasons in the K and L | spectral bands. |
| lasers requires the exponential growth of the | spectral bandwidth of gain and/or length of partial la |
| o be confused with the namesake SBasic (S for | Spectral Basic) Programming Language for the commercia |
| He is commander of the | Spectral Battle Beasts, one of the Seven Armies of the |
| urces for infrared spectroscopy because their | spectral behaviour corresponds approximately to that o |
| gnus' demonic knights and now an intimidating | spectral blue demonic aura, the demon Yamato, hovers a |
| designed to deliver photons with high average | spectral brightness in the 2 keV to 10 keV energy rang |
| trum to compare with other stars in a similar | spectral category. |
| f the progenitor, accounting for the observed | spectral changes. |
| Its | spectral characteristics are unknown. |
| The | spectral characteristics of the supernova changed over |
| s apparent magnitude +3.02 and belongs to the | spectral class K2 III. |
| Lambda Ophiuchi belongs to | spectral class A1V+A and has apparent magnitude +3.82. |
| J Centauri is a | spectral class B3V main sequence star with a mean appa |
| Classical Cepheids are yellow supergiants of | spectral class F6 - K2 and their radii change by (~25% |
| Misam belongs to the | spectral class K0 and has apparent magnitude +3.8. |
| The companion is a | spectral class M0.5V red dwarf star with absolute magn |
| d has an apparent magnitude of 2.72 and is of | spectral class K3, giving it a decidedly yellowish ora |
| Ardelean is a binary star, consisting of a | spectral class A2 giant with an apparent magnitude of |
| It has apparent magnitude +2.7 and belongs to | spectral class B2. |
| as apparent magnitude +3.1 and belongs to the | spectral class A0. |
| ive member has approximately 20 solar masses ( | spectral class O8 V). |
| Alchiba belongs to the | spectral class F0 and has apparent magnitude +4.00. |
| It is of | spectral class A3, and is approximately 99 light years |
| It is the closest | spectral class L brown dwarf to the Earth. |
| ary star is classified as a blue-white dwarf ( | spectral class B2.5 V). |
| Alpha Monocerotis belongs to the | spectral class G9 and is of apparent magnitude 3.93. |
| Miram belongs to | spectral class K3 and has an apparent magnitude of +3. |
| r is classified as a yellow-white supergiant ( | spectral class F8 Iab). |
| apparent magnitude of +3.5 and belongs to the | spectral class F0. |
| Gliese 435 (HD 101581, HIP 56998) is a K5 V e | spectral class stellar object located 40.9 light years |
| e star is classified as a yellow-white giant ( | spectral class F2 III). |
| It is an orange dwarf ( | spectral class K2V), somewhat dimmer and cooler than o |
| It is a red giant of the | spectral class M3, with a surface temperature of 3,650 |
| It belongs to the | spectral class T8V; its surface temperature is 600-750 |
| pparent magnitude of +2.88 and belongs to the | spectral class F2II. |
| f apparent magnitude +3.25 and belongs to the | spectral class M3-III. |
| It is a wide binary of | spectral class B stars, each of magnitude 4.0 and 5.1. |
| Its distance is about 108 light years and | spectral class is K1III. |
| Omega Herculis belongs to | spectral class B9pCr and has apparent magnitude +4.58. |
| Iota Leonis is of the | spectral class F4IV and apparent magnitude +3.94. |
| Ancha belongs to the | spectral class G8 and has an magnitude of +4.17. |
| considered normal for a main sequence star of | spectral class M. The proportion of elements with atom |
| The binary's composite | spectral class is F9V and its combined apparent magnit |
| Its | spectral class is intermediate between the C-type and |
| ittae B is a probably a substellar L dwarf of | spectral class L6±1.5 orbiting primary 15 Sagittae A. |
| Iota Ceti belongs to | spectral class K1.5III and has apparent magnitude +3.5 |
| Delta Scuti variables typically range from | spectral class A2 to F8, and a stellar luminosity clas |
| editors to change the category along with the | spectral class in the table. |
| y star system BD+31°643, which has a combined | spectral class of B5. |
| Gamma Ceti belongs to | spectral class A2 and has apparent magnitude +2.7. |
| he main sequence star is a red dwarf with the | spectral class M3.5V. |
| It belongs to the | spectral class T2.5 and its position shifts due to its |
| Eta Lyrae belongs to | spectral class B2.5IV and has apparent magnitude of +4 |
| Eta Pegasi is of | spectral class G2II-III and has apparent magnitude +3. |
| mers categorize it as a main-sequence star of | spectral class K2, which means the energy being genera |
| 41 Arietis belongs to the | spectral class B8Vn, and has a stellar magnitude of +3 |
| Persei has an apparent magnitude of +4.7 and | spectral class A2V. |
| Albali belongs to the | spectral class A0 and has an apparent magnitude of +3. |
| ht giant star of apparent magnitude +4.37 and | spectral class G1 II about 475 light years from Earth. |
| e enabled an observer to deduce the color and | spectral class of a star very easily. |
| 46 LMi has | spectral class K0+III-IV and is of magnitude 3.83. |
| Mu Leonis is of | spectral class K3 and apparent magnitude +4.1. |
| Sigma Puppis belongs to | spectral class K5 and has apparent magnitude +3.3. |
| maller and less luminous than our Sun, with a | spectral class of K3V, which makes it an orange-red hu |
| s apparent magnitude +4.67 and belongs to the | spectral class B3IV. |
| It has | spectral class M2 and is of apparent magnitude 3.5. |
| Alpha Equulei collectively belongs to | spectral class G0III and has apparent magnitude +3.92 |
| Alpha Hydri belongs to | spectral class F0V and has apparent magnitude +2.9. |
| o of 0.19 is too high, and it is of the wrong | spectral class to be part of the dark carbonaceous Hyg |
| Some Sun-like stars of | spectral class F8 to G8 have been found to undergo eno |
| Xi Geminorum belongs to | spectral class F6 and has apparent magnitude +3.4. |
| It belongs to the | spectral class T7, its surface temperature is 800-1300 |
| Beta Piscium belongs to the | spectral class B6Ve and is of magnitude +4.53m. |
| Each is of the | spectral class F7V and has a visual magnitude of 5.8m. |
| Earth, consisting of a magnitude 5.44 star of | spectral class M2 and a 6.6 magnitude star of spectral |
| It is an orange dwarf star of | spectral class K5, orbiting the yellow giant at about |
| 8 Aquarii is a blue-white sub-giant of the | spectral class A4IV in the constellation Aquarius with |
| Alpha Crateris belongs to the | spectral class K1, has apparent magnitude 4.07, and is |
| (absolute magnitude −0.7) and belongs to the | spectral class A0. |
| of +4.042 and is classified as a blue giant ( | spectral class O7.5III). |
| Gamma Librae belongs to the | spectral class K0III, and is of the fourth-magnitude, |
| The two stars of Subra are of | spectral class F9III (a giant star) for the primary an |
| d-magnitude) and is a blue giant belonging to | spectral class B8III. |
| light years from the Earth and belongs to the | spectral class B9.5V. |
| R Hydrae's | spectral class is M7IIIe. |
| It has a | spectral class of K1e and is located 39.9 light-years |
| a yellow star of apparent magnitude 3.88 and | spectral class F2 III about 61 light years from Earth. |
| visible to the naked eye, and belongs to the | spectral class B5III. |
| rateris is a white sub-giant belonging to the | spectral class A2, has apparent magnitude 4.48, and is |
| The | spectral class of the star is Am. |
| Persei has an apparent magnitude of +4.63 and | spectral class K1 III lying about 305 light years from |
| τ Pegasi belongs to the | spectral class A5Vp. |
| It has | spectral class A0 and is of magnitude 3.3. |
| The brightest companion, η Sagittarii B, is | spectral class F dwarf star, with an apparent magnitud |
| a yellow star of apparent magnitude 4.08 and | spectral class F6 III about 70 light years from Earth. |
| Gliese 349 is a star with a K3Ve | spectral class and a radial velocity of +27.6 km/s, lo |
| The spectrum matches a giant star of | spectral class G7Ib-II. |
| ghtness of +4.13 magnitude and belongs to the | spectral class F5IV; a subgiant star. |
| t was on the main sequence, it probably was a | spectral class B star (in the range B4-B9). |
| tar with an apparent magnitude of +3.17 and a | spectral class of B9. |
| Theta Cygni is a white main sequence star, | spectral class F3 V, forming a wide binary system with |
| The star is classified as a blue-white dwarf ( | spectral class B4 Vn). |
| It is a G-type giant star, with | spectral class G2 and an apparent visual magnitude of |
| aconis has apparent magnitude +3.75 and is of | spectral class K2-III. |
| 53 Eridani belongs to the | spectral class K2IIIb and has apparent magnitude +3.87 |
| The star is classified as an orange giant ( | spectral class K1 III). |
| lorum is a supergiant or bright giant star of | spectral class K5. |
| It contains many | spectral class O- and B-type stars, and may represent |
| Beta Aquilae has magnitude 3.71 and is of | spectral class G8IV. |
| This system consists of a | spectral class B3 star being orbited by a less massive |
| Gliese 208 is an orange dwarf star (K7 | spectral class) with an apparent magnitude of 8.9. |
| HIP 105766 is a potential Sun-like star (G5 | spectral class) with an apparent magnitude of 7.3. |
| liese 710 is a variable orange dwarf star (K7 | spectral class) in the constellation Serpens Cauda, wi |
| not expected to originate from a star of this | spectral class. |
| There is some uncertainty as to its | spectral class. |
| ally related to the group, being of the wrong | spectral class.Yet, NASA continues to categorize it as |
| The A6 part is the | spectral class: the A indicates this is a white star s |
| oped the system of classifying stars into the | spectral classes O, B, A, F, G, K, M. |
| evolution, along with main sequence stars of | spectral classes A, F, G, K, and M. |
| The movement of stars of | spectral classes B and A around the apex (left) and an |
| atoms and light related to the history of the | spectral classes. |
| If the | spectral classification is performed including the met |
| e main star is of apparent magnitude +1.6 and | spectral classification M4 III. |
| It has a | spectral classification of K2, giving it an orange-red |
| Spectral classification places it between a dwarf and | |
| apparent magnitude of +2.1 and belongs to the | spectral classification B3. |
| The MK system remains the standard stellar | spectral classification system used by astronomers tod |
| apparent magnitude of +1.5 and belongs to the | spectral classification B2. |
| White dwarfs whose primary | spectral classification is DA have hydrogen-dominated |
| ellman (1911-2007) to develop the MKK stellar | spectral classification system between 1939 and 1943. |
| It has a | spectral classification of K0 V and has about 86% of t |
| The Morgan-Keenan | spectral classification |
| Based on its | spectral classification of G0 V, it is similar in mass |
| n apparent magnitude of +2.08, belongs to the | spectral classification A5, and is about 47 light year |
| 2 stars are on the smaller end of the Harvard | spectral classification list, solely being larger than |
| The composite | spectral classification of the AB pair is G0V, which d |
| rked on problems of stellar statistics and on | spectral classification of stars, publishing the Bonn |
| that carbon and metals are not present, which | spectral classification is seen depends on the effecti |
| Its +6.4 magnitude white companion star ( | spectral classification A3) lies about 2 arcminutes aw |
| Its | spectral classification has been measured as A0 and al |
| e in brightness is accompanied by a change in | spectral classification, from G1 to F4. |
| Based on its | spectral classification, it is slightly less massive a |
| GJ 440 has a DQ | spectral classification, indicating that it is a rare |
| nent reddish-orange, well in keeping with its | spectral classification. |
| Measurement of the | spectral coherence of light requires a nonlinear optic |
| recious opal, where brilliant regions of pure | spectral color result from close-packed domains of col |
| A | spectral color is a color that is evoked by a single w |
| Every wavelength of light is perceived as a | spectral color, in a continuous spectrum; the colors o |
| While such a massive | spectral compilation itself was something of a tour de |
| spectral) complex impedance, equivalent to the amount | |
| xcipients, each of which will produce a Raman | spectral component with a relative intensity proportio |
| requires a method to separate the individual | spectral components and correlate their intensity cont |
| us signal and analyzing the resultant output, | Spectral Contamination testing provides a measure of a |
| and different sources of noise have different | spectral content. |
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