Variable Stars South. Who we are What we do. 2
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1
2 Who we are What we do 2
3 We are a group of amateur astronomers. Mainly from Australia New Zealand with a few from other parts of the globe We study stars that vary in brightness for one reason or another. We are project- based We cooperate with professionals as well as publishing papers on our own.
4 Visual observers Mk 1 eyeball Binoculars Telescope 4
5 Visual observers Mk 1 eyeball Binoculars Telescope Electronic detectors CCD/DSLR Photoelectric photometer Spectrometer 5
6 Visual observers Mk 1 eyeball Binoculars Telescope Electronic detectors CCD/DSLR Photoelectric photometer Spectrometer Data analysts Computer Internet Spreadsheet 6
7 Anyone can join It s FREE We accept donarons 7
8 Project based 8
9 Pulsa7ng Variables Miras Cepheids 9
10 Pulsa7ng Variables Miras Cepheids Eclipsing Variables EA (Algol type) EB (β Lyrae type) EW (W Uma type) 10
11 Pulsa7ng Variables Miras Cepheids Eclipsing Variables EA (Algol type) EB (β Lyrae type) EW (W UMa type) Cataclysmic Variables 11
12 Project - Dual maxima Miras Mira stars Oxygen or carbon rich On asymptorc giant branch of the H- R diagram Very large hundreds to thousands of R Cool K Luminous up to 10,000 L Large variability from 2.5 to 7 magnitudes Long periods hundreds of days Generally stable periods Subject to He shell flash 12
13 Light curve of Mira over 400 days 13
14 Period changes in R Hydrae since
15 Period changes in R Hydrae since
16 Visual light curve of R Normae made during the 1970s Graph from Stan Walker 16
17 UBV light curves of BH Crucis (Walker, W.S.G. JAAVSO Vol 37,2009) Period 421 days (1970s) Period 525 days (2000s) 17
18 Light curve of R Cen over 5000 days 18
19 Days Cycles Data from AAVSO provided by Stan Walker 19
20 Star RA Dec Max Min Period (days) Type Bo Comments R Centauri : V Mira 1.21 Prototype R Normae Mira 5.08 Prototype BH Crucis :V Mira 6.25 Evolved V Sra ~5 Strong duality Velorum BZ Carinae SRa Very probable TT Centauri Mira 1.90 Probable UX Circini Mira Like R Cru now BN Scorpii < Mira Probably not List of southern dual- maxima target stars 20
21 Star RA Dec Max Min Period (days) Type Bo Comments R Centauri : V Mira 1.21 Prototype R Normae Mira 5.08 Prototype BH Crucis :V Mira 6.25 Evolved V Sra ~5 Strong duality Velorum BZ Carinae SRa Very probable TT Centauri Mira 1.90 Probable UX Circini Mira Like R Cru now BN Scorpii < Mira Probably not List of southern dual- maxima target stars LX Cygni (dec +58) is an excellent northern hemisphere example of a Mira with a changing period 21
22 Project - Bright Cepheids Yellow or red supergiants On the Instability strip of HR diagram Massive 4-20 x M Very luminous up to 100,000 X L Periods from 2 to 40 days Magnitude change ~ 1mag PulsaRng caused by κ (kappa) mechanism - He ++ more opaque to radiaron than He
23 Project - Bright Cepheids Target stars suitable for DSLR photometry Magnitude < 9 Good historical background Period > 10 days Goals over 5 to 10 years Period changes Amplitude, shape of light curve Colour variarons 23
24 O C diagram of l (el) Carinae JD days Period change Julian days since (1870 to present) 24
25 Model light curve (red) of S Cru from ASAS data (blue points) Neil BuAerworth 25
26 Excel spreadsheet for finng MLC to seasonal light curve from DSLR photometry. (Neil BuAerworth) 26
27 O C for S Cru 1955 to 2013 showing no significant period change. (Neil BuAerworth) 27
28 Eclipsing variables EA (Algol type) detached, orbital plane 90 to line of sight. Do not change periods very much if at all. Mainly constant light between eclipses. 28
29 Eclipsing variables EA (Algol type) detached, orbital plane 90 to line of sight. Do not change periods very much if at all. Mainly constant light between eclipses. EB (β Lyrae type mainly semi- detached with at least one ellipsoidal component. SomeRmes difficult to specify exact Rmes of eclipse. One star filling Roche lobe. 29
30 Eclipsing variables EA (Algol type) detached, orbital plane 90 to line of sight. Do not change periods very much if at all. Mainly constant light between eclipses. EB (β Lyrae type) - mainly semi- detached with at least one ellipsoidal component. SomeRmes difficult to specify exact Rmes of eclipse. One star filling Roche lobe. EW (W UMa type) ellipsoidal components both overflowing Roche lobe. Depths of primary and secondary eclipse nearly equal, periods < 1 day. No constant light between eclipses. 30
31 Typical light curves of eclipsing binaries. (from hqp:// compas.belastro.net/bullern/issue/2/ p6) 31
32 Eclipsing variables Primary eclipse Brighter star is eclipsed by the fainter one. Eclipse is deepest. Secondary eclipse When fainter star is eclipsed by the brighter one. An eclipse is total if one star is completely obscured by the other for a period of Rme. Periods can change due to orbital precession, mass loss (wind) or mass transfer between the stars. 32
33 Project SPADES Search for Planets Around Detached Eclipsing Systems A pro- am project working with Simon O Toole Australian Astronomical Observatory 33
34 V0626 Sco an EA binary Phase 0.0 Phase 0.46 Light curve of V0626 Sco an EA binary with best fit line from Binary Maker 3 sorware David Moriarty 34
35 Some EAs were found to have small oscillarons similar to those of a delta ScuR star. (David Moriarty) HM Puppis Secondary Eclipse V magnitude Heliocentric Julian Day ( ) 35
36 GG Lup (1993) Light curve of eclipsing binary GG Lup 1985 (Andersen J., Clausen J.V., Giménez A., 1993 A&A, 277, 439) 36
37 Light curve of eccentric eclipsing binary GG Lup 2015 (Budding E., Butland R., Blackford M., MNRAS (April 21, 2015) Vol ). 37
38 GG Lup - an EB binary 38
39 Mark Blackford s dual DSLR photometry system. Canon EOS 1100D with 200mm f2.8 lens (6.5 x 4.3 ) Canon EOS 600D with 80mm f6 telescope (2.7 x 1.8 ) 39
40 EW binaries have quite short periods of 6 24 hours RV Gruis a contact binary p= 6.2 hrs. 40
41 hqp:// 41
42 Other projects Near IR photometry of Betelgeuse Too bright for professionals Three pulsaron periods: 2335, ~300, ~150 days Diameter changes Spectral type changes Candidate for type II Supernova mass 20M Many effects only visible in J & H bands (near IR) 42
43 Other projects Photometry of Red (M) Dwarfs 75% of stars in Milky Way Faint, small and old (maybe as old as the Galaxy) Project long- term monitoring of variability, rotaron and colour of selected RDs RotaRon periods 0.5 to 38 days Bright ones suitable for DSLRs Nine super- earths in habitable zone found from 102 southern RDs (Bonfils, X. et al, Astronomy & Astrophysics 549, A109) 43
44 44
45 Exoplanet Transit Database hqp://var2.astro.cz/etd/predicrons.php 45
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