Stars/Variables/Quiz

Variable stars is a lecture about variable stars.

You are free to take this quiz based on variable stars at any time.

To improve your score, read and study the lecture, the links contained within, listed under See also, External links, and in the template. This should give you adequate background to get 100 %.

As a "learning by doing" resource, this quiz helps you to assess your knowledge and understanding of the information, and it is a quiz you may take over and over as a learning resource to improve your knowledge, understanding, test-taking skills, and your score.

Suggestion: Have the lecture available in a separate window.

To master the information and use only your memory while taking the quiz, try rewriting the information from more familiar points of view, or be creative with association.

Enjoy learning by doing!

Quiz
{Complete the text: Capella B has a surface temperature of approximately { 5700 K (i) }, is spectral type { G0 III|G0III (i) }, has an orbital period with Capella A of about { 104 d|104.0217 d (i) }, and is a { RS Canum Venaticorum|RS CVn (i) } variable.
 * type="{}"}

{Which of the following is not a prominent contributor associated with a variable star? - star spots - chromospheric activity + rotation - brightness fluctuations - flares - spot coverage fraction
 * type=""}

{Main sequence variable stars of late spectral types, usually K or M, exhibiting variations in luminosity due to rotation, starspots and other chromospheric activity are called. { BY Draconis|BY Draconis variables (i) }
 * type="{}"}

{Yes or No, BH Centauri is an overcontact system. + Yes - No
 * type=""}

{Which of the following are associated with classical Cepheids as a standard candle? - characteristic mottling + young, disk objects + recent star formation - incipient resolution + pulsation phenomenon - easy to recognize + correction for absorption
 * type="[]"}

{True or False, RS Canum Venaticorum variables are close binary stars having active chromospheres which can cause large stellar spots. + TRUE - FALSE
 * type=""}

{Complete the text: Match up the type of star with each of the characteristics below: solar twin - A solar analog - B solar type - C double star - D binary - E visual binary - F astrometric binary - G spectroscopic binary - H eclipsing binary - I detached binary - J semidetached binary - K contact binary - L common-envelope binary - M area of gravitational pull exceeds the other component { J (i) }. same line of sight { D (i) }. wobbling around a point { G (i) }. no close companion with an orbital period of ten days or less { B (i) }. resolved binary using visual astronomy { F (i) }. periodic variation in radial velocity { H (i) }. each component fills the other's area of gravitational pull { L (i) }. F8V through K2V { C (i) }. unstable mass transfer from one to the other { M (i) }. mutual eclipses { I (i) }. two orbiting around each other { E (i) } no stellar companion { A (i) }. one component does not exceed the gravitational pull area { K (i) }.
 * type="{}"}

{Complete the text: Match up the likely type of star fission with each of the possibilities below: a triple-component stellar multiple - A massive star fission - B semidetached binary - C a separating close contact binary - D ZAMS system - E tight, circular orbit, impossible to tell eclipses - F lobate star - G coronal mass ejection - H BH Centauri { D (i) }. Plaskett's Star (HR 2422) { B (i) }. Betelgeuse { G (i) } W Ursae Majoris { F (i) }. Beta Lyrae { C (i) }. V1010 Ophiuchi { E (i) } object is confirmed to be co-moving { A (i) }. Sun { H (i) }.
 * type="{}"}

{Which of the following is a technetium star? - Alpha Camelopardalis + R Geminorum - TT CVn - S Camelopardalis - HR 107 - HR 774
 * type="[]"}

{Complete the text: Match up the likely type of star fission with each of the possibilities below: a triple-component stellar multiple - A massive star fission - B semidetached binary - C a separating close contact binary - D ZAMS system - E tight, circular orbit, impossible to tell eclipses - F lobate star - G coronal mass ejection - H BH Centauri { D (i) }. Plaskett's Star (HR 2422) { B (i) }. Betelgeuse { G (i) } W Ursae Majoris { F (i) }. Beta Lyrae { C (i) }. V1010 Ophiuchi { E (i) } object is confirmed to be co-moving { A (i) }. Sun { H (i) }.
 * type="{}"}

{Which of the following is a spectral class C or carbon star? - Alpha Camelopardalis + R Leporis + TT CVn + S Camelopardalis - Pistol Star + Y Canum Venaticorum
 * type="[]"}

{The type star that goes through fairly extreme changes of brightness: for instance, in 1952, its brightness increased by 75 times in only 20 seconds, is what star? { UV Ceti (i) }
 * type="{}"}

{Complete the text: Match up the observation with the binary star: Sirius A and B - A Algol A and B - B Albireo - C WISE J1049-5319 - D Mizar A - E Minkowski 2-9 - F { D (i) }. { A (i) }. { F (i) }. { C (i) }. { E (i) } { B (i) }.
 * type="{}"}

{Which of the following is not a spectral class M star? - Betelgeuse - Antares - Proxima Centauri - Barnard's star - VY Canis Majoris + Algol B
 * type=""}

{Which of the following is a spectral class S star? + BD Camelopardalis + S Ursae Majoris + Chi Cygni - Deneb - Altair - Fomalhaut
 * type="[]"}

Hypotheses

 * 1) The current metallicity of a star may depend on the presence of coronal clouds.