It is a " light irregular variable, changing its brightness erratically by about six percent . " ( It is technically known as an " Lb, " or " giant irregular, " variable ).
42.
Lambda Aquarii is a red giant star with a stellar classification of M2.5 III . It is classified as slow irregular variable and pulsation periods of 24.5, 32.0, and 49.5 days have been identified.
43.
"' Pulsating "'irregular giants or supergiants, called slow irregular variables, are all of late spectral types ( K, M, C, or S ), and classed as type L-LB for giants and LC for supergiants.
44.
The light curves of intrinsic variable stars with large amplitudes have been known for centuries to exhibit behavior that goes from extreme regularity, as for the classical Cepheids and the RR Lyrae stars, to extreme irregularity, as for the so-called Irregular variables.
45.
Other markings are formed of black irroration, namely four irregular patches along the dorsum, several irregular variable spots in the disc between the base and the middle, an elongate patch or streak margining the posterior costal patch beneath, and a streak along the upper part of the termen.
46.
Between these stars and Sirius lie K-type supergiant of spectral type K2.5Iab that is an irregular variable star, varying between apparent magnitudes 3.78 and 3.99 . Around 18 times as massive as the Sun, it shines with 65, 000 times its luminosity.
47.
RX Aurigae is a Cepheid variable as well; it varies in magnitude from a minimum of 8.0 to a maximum of 7.3; its spectral class is G0Iabv . It has a period of 11.62 days . RW Aurigae is the prototype of its class of irregular variable stars.
48.
On early 20th century and older orthochromatic ( blue-sensitive ) photographic film, the relative brightnesses of the blue supergiant Rigel and the red supergiant Betelgeuse irregular variable star ( at maximum ) are reversed compared to what human eyes perceive, because this archaic film is more sensitive to blue light than it is to red light.
49.
The MK spectral type of V424 Lac has been determined to be K5, Multiple short periods are detected, as well as slow variations with a period of 1, 100 or 1, 601 days . Although listed in the General Catalogue of Variable Stars as a slow irregular variable, it has been considered to be either a semiregular variable or long secondary period variable.
50.
The star system shows regular variations in brightness that were reported as a 97.5 day period in the Hipparcos catalogue, Although the light curve appears to show eclipses, the high orbital inclination suggests the variations are due to ellipsoidal stars as they rotate in their orbit . ? Phoenicis is listed in the General Catalogue of Variable Stars as a possible slow irregular variable with a range from 3.39 to 3.49, the same as reported for the eclipses or ellipsoidal variations.
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