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Topic: Semiregular variable

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	CONK! Encyclopedia: Variable_star (Site not responding. Last check: 2007-11-06)
		Variable stars are generally analysed using photometry and photospectrometry.
		For regular variables, the period of variation and its amplitude can be very well established; for many variable stars, though, these quantities may vary slowly over time, or even from one period to the next.
		This variation is thought to be caused by episodes of dust formation in the atmosphere of the star.
	www.conk.com /search/encyclopedia.cgi?q=Variable_star (1394 words)

	Semiregular variable star - Wikipedia, the free encyclopedia
		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.
		Amplitudes and light-curve shapes generally vary and periods are in the range of 35-1200 days.
		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.
	en.wikipedia.org /wiki/Semiregular_variable_star (345 words)

	GCVS3
		For the eclipsing variables and the RV Tauri type stars the epoch of the minimum brightness is given, while for all the variable stars of other types, the epochs of maximum is given.
		Semiregular variable supergiants of late spectral classes, representatives of the flat component of the Galaxy (e.g., m Cep, RS Cnc).
		RR Lyrae variables (short-period cepheids, or cluster variables).
	www.to.astro.it /astrometry/Astrometry/DIRA2/DIRA2_doc/GCVS/GCVS3.HTML (2571 words)

	[No title] (Site not responding. Last check: 2007-11-06)
		00 18.4 +44 01 GRB 34 + A is a BY Dra-type variable, CQ And, and a 00 18.4 +44 01 GRB 34 spectroscopic binary.
		A is a variable of the Alpha CVn type, 02 26.0 -15 20 H 80 AB Cet, and a spectroscopic binary.
		A is a specroscopic binary and variable, 04 22.1 +14 05 BUP 54 V775 Tau.
	xml.gsfc.nasa.gov /pub/adc/xml_archives/catalogs/1/1237/1237_notes.dat (19590 words)

	Semiregular variable star -- Facts, Info, and Encyclopedia article (Site not responding. Last check: 2007-11-06)
		The amplitudes may be from several hundredths to several (The property of relative size or extent) magnitudes (usually 1-2 magnitudes in the V filter).
		Semiregular (A quantity that can assume any of a set of values) variables are classified in several subtypes:
		SRA: Late spectral-type (M, C, S or Me, Ce, Se) giants displaying persistent periodicity and usually small amplitude, less than 2.5 (The property of relative size or extent) magnitudes in V. Z Aquarii is an example of this class.
	www.absoluteastronomy.com /encyclopedia/s/se/semiregular_variable_star.htm (386 words)

	[No title]
		These variables probably mark one of the evolutionary stages of T Tauri-type Orion variables (INT), as evidenced by an outburst of one member, V1057 Cyg, but its decline (2.5 mag in 11 years) commenced immediately after maximum brightness was attained.
		The period of variation is close to the orbital one, and the variability amplitude is usually as great as 0.2 mag in V (UX Ari).
		The variability of the wave's amplitude (which may be up to 0.2 mag in V) is explained by the existence of a long-period stellar activity cycle similar to the 11-year solar activity cycle, during which the number and total area of spots on the star's surface vary.
	astro.u-szeged.hu /ismeret/valtozok/vartype.txt (4698 words)

	AAVSO: Variable Star of the Month, Z Uma
		General Catalogue of Variable Stars (GCVS) Z UMa is recorded to vary in brightness from its faintest minimum magnitude of 9.4 to its brightest maximum magnitude of 6.2.
		The variable star, Z UMa, sits in the bowl of the The Big Dipper, nearly 3 degrees west-northwest of the star “delta”, which connects the handle to the bowl of the dipper.
		Mira and semiregular variables are pulsating low and intermediate mass "red variables" that occupy a distinct zone in the far right region on the HR diagram.
	www.aavso.org /vstar/vsots/0300.shtml (1619 words)

	[No title]
		A is a BY Dra-type variable, CQ And, and a spectroscopic binary.
		A is VW Ari, a Delta Scuti-type variable.
		A is a spectroscopic binary and variable, V776 Tau.
	ad.usno.navy.mil /wds/wds1996/wds1996notes_main.txt (17340 words)

	V Boo, an SR of declining amplitude
		Therefore the conclusion is that, like some other semiregular variables, V Boötis' lightcurve is best represented by two periodicities: a main one of 257.8 days and a minor one of 137.1 days.
		From the amplitude spectrum both signals are quite stable, although the main one may show some slight variation, as indicated by the dispersion of some of the amplitude in Figures 3 and 4 to periodicities around the 259 day mark.
		Therefore, despite some suggestion of varying periodicity, further investigation reveals that it is no more than the scatter to be expected from a semiregular star, and indeed is quite stable for such a star.
	www.britastro.org /vss/00042b.html (1601 words)

	VizieR Complement
		R Semiregular variables, which are giants or supergiants of intermediate and late spectral types showing noticeable periodicity in their light changes, accompanied or sometimes interrupted by various irregularities.
		RB Semiregular late-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, and even with light constancy intervals (RR CrB, AF Cyg).
		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 (SX Her, SV UMa).
	cdsweb.u-strasbg.fr /viz-bin/vizExec/Vgrep?II/214A&-p&-pre&-s:&^S:&vartype.txt (678 words)

	Read about Semiregular variable star at WorldVillage Encyclopedia. Research Semiregular variable star and learn about ... (Site not responding. Last check: 2007-11-06)
		supergiants of intermediate and late spectral type showing considerable periodicity in their light changes, accompanied or sometimes interrupted by various irregularities.
		light curves may be rather different and variable with each cycle.
		SV Ursae Majoris are examples of this class.
	encyclopedia.worldvillage.com /s/b/Semiregular_variable (356 words)

	Examples of TASS Mark III Data
		One of the known variable stars which falls within our survey area is the star X Ceti, at RA = 49.8569 degrees and Dec = -1.0660 degrees.
		This is a star that Michael had one period of on his AAS poster paper and I think now it has been determined as a new semi-regular that two periods of the star have been recorded.
		The known variable TW Aqr is just a short distance away from BD -02 5436 -- see its light curve in the next section.
	www.tass-survey.org /tass/data/data_iii.html (1089 words)

	Evolution of #tex2html_wrap_inline1152# maser emission in the direction of the semiregular variable RT Virginis during ... (Site not responding. Last check: 2007-11-06)
		Evolution of #tex2html_wrap_inline1152# maser emission in the direction of the semiregular variable RT Virginis during 1985-1996
		The characteristic time variation of the maser emission at each of these groups was about 5-6 years.
		This phenomenon may be explained by a variation of the outflow of the matter from the star.
	www.edpsciences.org /journal/index.cfm?v_url=aas/full/1997/17/ds1238/ds1238.html (261 words)

	RV Tauri star Comparison Table (Site not responding. Last check: 2007-11-06)
		A class of giant and supergiant pulsating stars of spectral class M, K, N, R, or S with a periodic (or semiperiodic) light curve of varying amplitude.
		A class of about 100 semiregular variable yellow supergiants of late spectral type (G-K), similar to W Virginis stars but with longer periods.
		Their spectra often contain emission lines, and their light curves have alternating deep and shallow minima.
	www.csi.uottawa.ca:4321 /astronomy/RVTauristar_table.html (105 words)

	Astron. Astrophys. 343, 241-250 (1999) (Site not responding. Last check: 2007-11-06)
		O maser emission region for semiregular variables is an ellipsoidally-shaped shell.
		The velocity of RT Vir was estimated by Bowers and Johnston (1994).
		O maser emission toward the semiregular variable RT Vir, undertaken by Mendoza-Torres et al.
	aa.springer.de /papers/9343001/2300241/sc1.htm (667 words)

	1 Introduction (Site not responding. Last check: 2007-11-06)
		OH semiregular variable stars (SRs) appear to be an extreme class of such objects where circular polarisation reached up to 55-75%, even for spectra obtained with a moderate resolution (Szymczak et al.
		The general properties of the OH variations in these stars were recently reported in Paper I (Etoka et al.
		These data provide the first conclusive evidence for variations in the net circular polarisation, the degree of fractional polarisation, and a relationship between linear and circular polarisations.
	aanda.u-strasbg.fr:2002 /papers/aa/full/2001/45/aa1719/node1.html (399 words)

	[75.06] Mass-Losing Semiregular Variable Stars in Baade's Windows (Site not responding. Last check: 2007-11-06)
		Using the MACHO lightcurves, we classify the majority of these stars as semiregular variables.
		This is the first large sample of semiregular variable stars whose pulsation and mass-loss rates are well-characterized, and whose distances, and thus energetics, are also known.
		We find that luminosity, mass-loss rate, and pulsation period are correlated, in the sense that semiregulars with higher luminosities and higher mass-loss rates have longer periods.
	www.aas.org /publications/baas/v31n5/aas195/762.htm (258 words)

	Wavelet papers
		Szatmáry K., Vinkó J.: 1992, Periodicities of the light curve of the semiregular variable
		Gál J., Szatmáry K.: 1995, Mode switching in red semiregular variable stars?, Proc.
		The semiregular star V Bootis, Astronomy and Astrophysics 308, 791-798.
	astro.u-szeged.hu /kutatas/wavelet.html (438 words)

	VizieR Complement
		Many type L variables are really semiregulars or belong to other types.
		SR Semiregular variables, which are giants or supergiants of intermediate
		vary and periods are in the range of 35-1200 days.
	cdsweb.u-strasbg.fr /viz-bin/vizExec/Vgrep?II/214A&-p&...&vartype.txt (5657 words)

	[8.01] Secular evolution in Mira and semiregular variable star pulsations (Site not responding. Last check: 2007-11-06)
		The Mira and semiregular variables are pulsating stars in very advanced stages of evolution, and they exhibit a wide variety of pulsation behavior.
		It is suspected that a small number of these variables (including R Aql, R Hya, T UMi, and LX Cyg) are exhibiting large, secular period changes due to structural readjustments from recent thermal pulses.
		Analysis of secular period changes and other changes in pulsation behavior may therefore be useful in studies of the evolution of these stars.
	www.aas.org /publications/baas/v35n5/aas203/547.htm (240 words)

	Mira Information from AAVSO
		Mira-type variable stars are cool red giant stars that are named for the prototype of the class, omicron Ceti, or more commonly known as Mira.
		(See the December 1998 VSOTM for Mira.) Such variables are found in the high luminosity portion of the asymptotic giant branch (AGB) in the H-R diagram, along with the semiregular variable stars.
		(For a review of the semiregular variable stars, see the March 2000 and December 2000 VSOTM for Z Ursae Majoris and Betelgeuse, respectively.) In comparison with solar parameters, stars belonging to the Mira membership of variable stars generally have larger radii, higher luminosities, lower temperatures, and lower surface gravities than our Sun.
	isi.ssl.berkeley.edu /aavso_mira_information.htm (1020 words)

	[No title]
		The new variability types (ZZO, AM, R, BE, LBV, BLBOO, EP, SRS, LPB) have been added in the Name-Lists 67- 77 and in the GCVS vol.V. ZZO ZZ Cet type variables of the DO spectral type showing HeII and and CIV absorpion lines in their spectra.
		SRS Semiregular pulsating red giants with short period (one month), probably high-overtone pulsators.
		Distribution Statistics of Designated Variable Stars According to their Types of Variability (GCVS I-III and NL 67 - 77).
	www.sai.msu.su /groups/cluster/gcvs/gcvs/iii/vartype.txt (4745 words)

	Variable star (Site not responding. Last check: 2007-11-06)
		Double stars are generally analysed using photometry and photospectrometry.
		One of the most famous eclipsing binaries is Algol, or Beta Persei.
		Stars with planetary systems may also show brightness variations if their planets pass between the earth and the star.
	www.worldhistory.com /wiki/V/Variable-star.htm (1132 words)

	Constellation Perseus
		An attractive pair for small telescopes is eta Per: a red and a blue star of 4th and 9th mag sitting in a star rich field.
		During the eclipsing phase the brightness varies from 2.2 mag to 3.5 mag.
		The brightness of the variable star rho Per varies semiregularily from 3rd mag to 4th mag.
	www.seds.org /Maps/Stars_en/Fig/perseus.html (591 words)

	Masi Astro_images_var (Site not responding. Last check: 2007-11-06)
		South is up and west to the left in these images.
		to have a period of variation of some months.
		that it's a semiregular variable with a cycle-length of a few months.
	www.bellatrixobservatory.org /skiff.html (285 words)

	Catalogue: J/ApJ/552/289
		J/ApJ/552/289 Semiregular variable stars in Baade's windows (Alard+, 2001) ================================================================================ Mass-losing semiregular variable stars in Baade's windows.
		ISOGAL mid-infrared photometry (7 and 15µm and MACHO V and R light curves are assembled for approximately 300 stars in the Baade's windows of low extinction toward the Galactic bulge.
		This file × table1.dat 102 332 Summarized photometry of sources × table2.dat 64 14 Mira variables in the survey area × table3.dat 69 26 Spectral energy distribution modeling results
	cdsweb.u-strasbg.fr /cgi-bin/Cat?J/ApJ/552/289 (709 words)

	AAVSO: S-Z Subject Index of Journal of the AAVSO (JAAVSO)
		Statistical Analysis of the Semiregular Variable AR Cephei {A. Kucinskas} 19.73
		Variability of W Cygni (Abs.) {R. Schmude, Jr.
		Classification of the Enigmatic Nantucket Variable XX Sct {Jessica Bonjorni and Nikolai Samus} 28.87
	www.aavso.org /publications/journal/s-z.shtml (3852 words)

	Learn more about List of semiregular variable stars in the online encyclopedia. (Site not responding. Last check: 2007-11-06)
		Learn more about List of semiregular variable stars in the online encyclopedia.
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	www.onlineencyclopedia.org /l/li/list_of_semiregular_variable_stars.html (105 words)

	Betelgeuse Comparison Table (Site not responding. Last check: 2007-11-06)
		physical object > natural object > celestial body > star > late star > semiregular variable > Betelgeuse
		A supergiant with spectral type M. Red supergiants are the largest stars in the universe: if put in place of the Sun, some would touch Saturn.
		Betelgeuse is also a strong infrared emitter - at 2 µ the brightest in the sky.
	www.csi.uottawa.ca:4321 /astronomy/Betelgeuse_table.html (271 words)

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