Matches in DBpedia 2016-04 for { <http://wikidata.dbpedia.org/resource/Q1054411> ?p ?o }
Showing triples 1 to 26 of
26
with 100 triples per page.
- Q1054411 subject Q8729026.
- Q1054411 abstract "Semiregular variable stars are giants or supergiants of intermediate and late spectral type showing considerable periodicity in their light changes, accompanied or sometimes interrupted by various irregularities. Periods lie in the range from 20 to more than 2000 days, while the shapes of the light curves may be rather different and variable with each cycle. The amplitudes may be from several hundredths to several magnitudes (usually 1-2 magnitudes in the V filter).Semiregular variables are classified in several subtypes:SRA: Spectral-type (M, C, S or Me, Ce, Se) giants displaying persistent periodicity and usually small amplitude, less than 2.5 magnitudes in V. R Doradus and RX Leporis are examples of this class. Amplitudes and light-curve shapes generally vary and periods are in the range of 35–1200 days. Many of these stars differ from Mira variables only by showing smaller light amplitudes, and they are essentially Mira variables pulsating in an overtone, while the Miras themselves pulsate in a fundamental mode.SRB: Spectral-type (M, C, S or Me, Ce, Se) giants with poorly defined periodicity (mean cycles in the range of 20 to 2300 days) or with alternating intervals of periodic and slow irregular changes. Some may occasionally cease varying at all for a time. RR Coronae Borealis and T Centauri are examples of this behavior. Every star of this type may usually be assigned a certain mean period. In a number of cases, the simultaneous presence of two or more periods of light variation is observed.SRC: Spectral-type (M, C, S or Me, Ce, Se) supergiants with amplitudes of about 1 mag and periods of light variation from 30 days to several thousand days. Mu Cephei and Betelgeuse are bright examples of this class.SRD: Giants and supergiants of F, G, or K spectral types, sometimes with emission lines in their spectra. Amplitudes of light variation are in the range from 0.1 to 4 mag, and the range of periods is from 30 to 1100 days. V810 Centauri is an example of this class. The globular cluster M13 contains a dozen red variable stars from 11.95 to 12.25 visual magnitude, and with period of 43 days (V24) to 97 days (V43).↑ ↑".
- Q1054411 wikiPageExternalLink 0701.shtml.
- Q1054411 wikiPageWikiLink Q11276.
- Q1054411 wikiPageWikiLink Q11312.
- Q1054411 wikiPageWikiLink Q115379.
- Q1054411 wikiPageWikiLink Q12124.
- Q1054411 wikiPageWikiLink Q124313.
- Q1054411 wikiPageWikiLink Q13781.
- Q1054411 wikiPageWikiLink Q179600.
- Q1054411 wikiPageWikiLink Q193599.
- Q1054411 wikiPageWikiLink Q3508433.
- Q1054411 wikiPageWikiLink Q4181312.
- Q1054411 wikiPageWikiLink Q50081.
- Q1054411 wikiPageWikiLink Q5097781.
- Q1054411 wikiPageWikiLink Q5098357.
- Q1054411 wikiPageWikiLink Q5175907.
- Q1054411 wikiPageWikiLink Q573.
- Q1054411 wikiPageWikiLink Q593448.
- Q1054411 wikiPageWikiLink Q6243.
- Q1054411 wikiPageWikiLink Q6692732.
- Q1054411 wikiPageWikiLink Q675076.
- Q1054411 wikiPageWikiLink Q744691.
- Q1054411 wikiPageWikiLink Q8729026.
- Q1054411 comment "Semiregular variable stars are giants or supergiants of intermediate and late spectral type showing considerable periodicity in their light changes, accompanied or sometimes interrupted by various irregularities. Periods lie in the range from 20 to more than 2000 days, while the shapes of the light curves may be rather different and variable with each cycle.".
- Q1054411 label "Semiregular variable star".