「SPECTROSCOPIC」の共起表現一覧(2語左が「is」)
該当件数 : 56件
| Component A is a | spectroscopic binary. |
| HD 37017 is a | spectroscopic binary. |
| Lambda Virginis is a | spectroscopic binary. |
| IU Aurigae is a | spectroscopic binary. |
| EZ Aquarii AC is a | spectroscopic binary. |
| rimary component, Epsilon Volantis A, is a | spectroscopic binary. |
| 3 Camelopardalis is a | spectroscopic binary in the constellation Camelopardalis |
| 12 Camelopardalis is a | spectroscopic binary in the constellation Camelopardalis |
| V373 Cas is a | spectroscopic binary in the constellation Cassiopeia. |
| V357 Carinae (a Car, a Carinae) is a | spectroscopic binary in the constellation Carina. |
| Theta-1 Sagittarii is a | spectroscopic binary lying 617 light years from Earth. |
| θ1 Crucis (θ1 Cru, Theta1 Crucis) is a | spectroscopic binary star in the constellation Crux. |
| The star e Serpentis (e Ser) is a | spectroscopic binary in the constellation of Serpens. |
| It is a | spectroscopic binary whose components have an orbital pe |
| It is a | spectroscopic binary whose components have an orbital pe |
| It is a | spectroscopic binary with an orbital period of 143.6065 |
| Pi Andromedae (π And, π Andromedae) is a | spectroscopic binary in the constellation Andromeda. |
| It is a | spectroscopic binary and has a companion located 0.12 ar |
| Secondary, Σ 1694 B is a | spectroscopic binary both A-type main sequence star. |
| It is a | spectroscopic binary whose two components are separated |
| 104 Aqr A is a | spectroscopic binary and is suspected to be variable. |
| Lambda Andromedae is a | spectroscopic binary with an orbital period of 20.52 day |
| It is a | spectroscopic binary with an orbital period of 134 days. |
| θ2 Crucis (θ2 Cru / Theta2 Crucis) is a | spectroscopic binary star in the constellation Crux. |
| Zeta Trianguli Australis (ζ TrA) is a | spectroscopic binary in the constellation Triangulum Aus |
| It is a | spectroscopic binary whose components have magnitudes of |
| Pi4 Orionis (π4 Ori, π4 Orionis) is a | spectroscopic binary star in the constellation Orion. |
| It is a | spectroscopic binary, whose components are separated by |
| It is a | spectroscopic binary with a faint class-G companion. |
| 17 Leporis (17 Lep) is a | spectroscopic binary star in the constellation of Lepus. |
| ilon Sagittarii (υ Sgr, υ Sagittarii) is a | spectroscopic binary star system in the constellation Sa |
| The primary is a | spectroscopic binary, and its close companion completes |
| Theta Aquilae is a | spectroscopic binary classified as a blue-white B-type g |
| omponent, Iota Trianguli Australis A, is a | spectroscopic binary with a mean apparent magnitude of + |
| Iota Arietis is a | spectroscopic binary classified as a yellow G-type super |
| It is a | spectroscopic binary with components that are too close |
| anis Majoris (ζ CMa, ζ Canis Majoris) is a | spectroscopic binary in the constellation Canis Major. |
| Gliese 678 is a | spectroscopic binary star system approximately 60 light- |
| This is a | spectroscopic binary, which means that the individual co |
| HD 176051 is a | spectroscopic binary star system located approximately 4 |
| This star is a | spectroscopic binary, and the primary is also a Beta Cep |
| is its very high basicity; another is its | spectroscopic properties. |
| omedae (Eta And, η Andromedae, η And) is a | spectroscopic binary star in the constellation of Androm |
| Linear dichroism (LD) is a | spectroscopic technique that is primarily used to study |
| Rho Tucanae is a | spectroscopic binary composed of two yellow-white F-type |
| It is a | spectroscopic binary, and the two subcomponents have app |
| Chi Aurigae is a | spectroscopic binary which is classified as a blue-white |
| It is a | spectroscopic binary, which means it is a binary star wi |
| name HR 2422 Monocerotis or HR 2422) is a | spectroscopic binary at a distance of around 6600 light- |
| Atik is a | spectroscopic binary star consisting of a spectral type |
| It is a | spectroscopic binary having a 113.8 day period, indicati |
| Kappa Arietis is a | spectroscopic binary which is classified as a white A-ty |
| Reflectance difference spectroscopy is a | spectroscopic technique which measures the difference in |
| l magnitude of approximately 5.15 and is a | spectroscopic binary star which consists of two giant st |
| The Rossiter-McLaughlin effect is a | spectroscopic phenomenon observed when either an eclipsi |
| At the centre of the system is a | spectroscopic binary, Iota Serpentis A and B. These are |
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