「spectral」の共起表現(1語右で並び替え)

「spectral」の共起表現一覧(1語右で並び替え)

spectral

1 2 3 4 次へ＞

1語右で並び替え

該当件数:734件

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.

1 2 3 4 次へ＞