Cefeidy Gieren et al., arXiv:astro-ph/0503637 v1 29 Mar 2005 RR Gem (jurcsik et al., 2005, P=7d, the shortest Blazhko) V 10.69 V473 Lyr (Amplitude variability of the cepheid V473 Lyr, Breger, M., Communications in Asteroseismology, vol.148, p. 52-56, 2006, Equidistant frequency triplets in pulsating stars: the combination mode hypothesis, Breger, M.; Kolenberg, K. , Astronomy and Astrophysics, Volume 460, pp.167-172 3 Vul, A Photometric and Spectroscopic Study of 3 Vulpeculae: An Observer's Nightmare, Robert J. Dukes, Jr., William R. Kubinec, Angela Kubinec, and Saul J. Adelman, 2003, The Astronomical Journal, 126, 370–384 2 Galactic Cepheids are 1st/2nd overtone double-mode pulsators: CO Aur, HD 304373 3 Triple-Mode variables: AC And, V829 Aql, V823 Cas Two modes: High amplitude -> radial Not a standard ratio Binary variables? No: linear combination modes! V371 Per Cepheid Periods 1.27 and 1.74 days Ratio 0.73 V767 Sgr Cepheid? Periods 0.54 and 0.67 days Ratio 0.80 (< 1st/2nd overtone) HADS: GSC 4311-825: 1 radial + 2 non-radial modes M13, Kopacki (2005) -rozne pulsujace Evans et al, 2005 (18 binary cepheids) CO Aur V 7.73, P=1.78, 1.42d UBV photoelectric photometry of the 1H/2H double mode cepheid CO Aurigae, Santangelo, M. M. M.; Cavalletti, G.; Benedetti, W., Astronomische Nachrichten, 328, 55. S.V. ANTIPIN1, N.A. GORYNYA2 et al, IBVS 4718, BD -10°4669, CO Aur, TU Cas, EW Sct, V367 Sct, and BQ Ser. Mean Angular Diameters and Angular Diameter Amplitudes of Bright Cepheids, P. Moskalik, N. A. Gorynya, Acta Astron. 55, 247 Masses for Galactic Beat Cepheids, D'Cruz, Noella L.; Morgan, Siobahn M.; Böhm-Vitense, Erika, Astronomical Journal, 120, 990 Polaris, Polaris: Amplitude, Period Change, and Companions, Nancy Remage Evans, Dimitar D. Sasselov, and C. Ian Short, 2002, ApJ 567, 1121 The Period Changes of Polaris , Turner, David G.; Savoy, Jonathan; Derrah, Jayme; Abdel-Sabour Abdel-Latif, Mohamed; Berdnikov, Leonid N. PASP 117, 207 Extended envelopes around Galactic Cepheids. II. Polaris and ? Cephei from near-infrared interferometry with CHARA/FLUOR, Mérand, A.; Kervella, P.; Coudé Du Foresto, V.; Perrin, G.; Ridgway, S. T.; Aufdenberg, J. P.; Ten Brummelaar, T. A.; McAlister, H. A.; Sturmann, L.; Sturmann, J.; Turner, N. H.; Berger, D. H., 2006, A&A 453, 155 Gromady otwarte Karchenko et al. 2005 Catalogue of open clusters Ahumada, J. A.; Lapasset, E., New catalogue of blue stragglers in open clusters, 2007A&A...463.. A&A 376, 441-447 (2001), Proper motions of open clusters within 1 kpc based on the TYCHO2 Catalogue, W. S. Dias - J. R. D. Lépine - B. S. Alessi arXiv:astro-ph/0309232 v1 8 Sep 2003 (pozycje i odleglosci) www.ctio.noao.edu/REU/ctioreu_2006/work/allison.pdf Variable stars in the field of open cluster NGC 6819 http://www.astro.keele.ac.uk/~jkt/pubs/Southworth-proc-IAUS240.pdf (southworth, list of solutions) Street R.A.1; Horne K.; Lister T.A.1; Penny A.2; Tsapras Y.1; Quirrenbach A.3; Safizadeh N.3; Cooke J.3; Mitchell D.3; Collier Cameron A., Monthly Notices of the Royal Astronomical Society, Volume 330, Number 3, March 2002, pp. 737-754 www.aanda.org/articles/aa/pdf/2001/35/aah2757.pdf (M37, poor photometry, 2 candidate eclipsing binaries) A&A 371, 571-578 (2001), Search for short-period variable stars in the open cluster NGC 2301, S.-L. Kim et al. (5 eclipsing, UBVI) Eclipsing binaries in open clusters - III. V621 Per in ? Persei, Southworth, J.; Zucker, S.; Maxted, P. F. L.; Smalley, B., Monthly Notices of the Royal Astronomical Society, Volume 355, Issue 3, pp. 986-994 Plejady A distance of 133-137 parsecs to the Pleiades star cluster, Pan, Xiaopei; Shao, M.; Kulkarni, S. R., Nature, Volume 427, Issue 6972, pp. 326-328 (2004). A purely geometric distance to the binary star Atlas, a member of the Pleiades, Zwahlen, N.; North, P.; Debernardi, Y.; Eyer, L.; Galland, F.; Groenewegen, M. A. T.; Hummel, C. A., Astronomy and Astrophysics, v.425, p.L45-L48 (2004) The distance to the Pleiades from orbital solution of the double-lined eclipsing binary HD 23642, Munari, U.; Dallaporta, S.; Siviero, A.; Soubiran, C.; Fiorucci, M.; Girard, P., Astronomy and Astrophysics, v.418, p.L31-L34 (2004) Eclipsing binaries as standard candles. HD 23642 and the distance to the Pleiades , Southworth, J.; Maxted, P. F. L.; Smalley, B., Astronomy and Astrophysics, v.429, p.645-655 (2005) M.A.T. Groenewegen, Decin, Salaris, De Cat, 2007, A&A in press Valls-Gabaud et al., in prep DEBs Kelley, N., Shaw, J.S., combined NSVS/2mass database search for cool algols and eclipsing subdwarfs Pulsating components of eclipsing binaries in the ASAS-3 catalog A. Pigulski, G. Michalska, Acta Astronomica HD 220687 23 25 47.819 -11 36 35.67 V 9.55 P=1.5942 f=26.169254 IBVS.5669, 2005, Kim, S.-L.; Lee, C.-U.; Koo, J.-R.; Kang, Y. B.; Lee, J. W.; Mkrtichian, D. E., Discovery of a Short-Periodic Pulsating Component in the Algol-Type Eclipsing Binary System IV Cas BVRJK Photometry and a Spectroscopic Study of the Algol Short-Period Binary VV Ursae Majoris, Lázaro, C.; Arévalo, M. J.; Martínez-Pais, I. G.; Domínguez, R. M., AJ 123, 2733, 2002 On a short-periodic pulsating component in the Algol-type eclipsing binary system VV UMa Kim, S.-L.; Lee, J. W.; Lee, C.-U.; Kang, Y. B.; Koo, J.-R.; Mkrtichian, D. E., IBVS 5598, 2005 VV UMa 09 38 06.722 +56 01 07.27 V 10.28 P=0.687d f=50c/d AB Cas -- Eclipsing binary of Algol type/DSCT P=1.366d f=20c/d, 02 37 31.514 +71 18 16.26, V 10.32, MNRAS 353, 310 RX Hya 09 05 41.16 -08 15 39 V 9.5 P= 2.28d f=19.39 AB Per 03 37 45.203 +40 45 49.38 P=7.16d f1 = 0.747 c/d, f2 = 5.106 c/d and f3 = 2.624 c/d. V440 Per 02 23 51.744 +55 21 53.50, V 6.300, P=7.7d (classical cepheid with weak 2nd harmonics) ===================================================================================== From pam@camk.edu.pl Wed Mar 28 17:20:02 2007 Date: Wed, 28 Mar 2007 17:20:00 +0200 (CEST) From: Pawel Moskalik To: Aleksander Schwarzenberg-Czerny Cc: Pawel Moskalik Subject: V473 Lyr i V440 Per 1 - star 2 - period(s) 3 - number of velocity measurements 4 - source of velocity measurements 5 - type: D - double mode CF - classical fundanental Cs - classical overtone CW - Pop II 6 - binarity/orbital period 7 - orbital amplitude K [km/s] 8 - source of orbital information 9 - detection of period change 10 - source of period change information ============================================================================ == 1 2 3 4 5 6 7 8 9 10 ============================================================================ == V473 Lyr 1.49101 9 1 C yes 161 246 2 167 17 3 177 52 4 40 5 150 6 ============================================================================ == 1. Percy, J. R. & Evans, N. R. 1980, Astron. J., 85, 1509. 2. Burki, G., Mayor, M. & Benz, W. 1982, Astron. Astrophys., 109, 258. 3. Arellano Ferro, A. 1984, MNRAS, 209, 481. 4. Burki, G. et al. 1986, Astron. Astrophys., 168, 139. 5. Gorynya, N. A., Samus, N. N., Sachkov, M. E., Rastorguev, A. S., Glushkova, E. V. & Antipin, S. V. 1998, Pisma Astron. Zh., 24, 939 (Astron. Lett., 24, 815). 6. Gorynya 4 (unpublished). Teraz o V440 Per: polamplituda pulsacji A1=2.62+-0.08km/s polamplituda harmonika A2=0.25+-0.08km/s okres pulsacji P=7.57183day jasnosc gwiazdy =6.28mag Celem obserwacji jest zmierzenie A2 z jak najlepsza dokladnoscia. Pozadana dokladnosc: 0.04km/s badz lepiej. Oceniam, ze przy dokladnosci pojedynczego pomiaru rownej 0.25km/s, potrzeba bedzie 70-100 pomiarow. 12 Apr 2007-Unaczesnienie od PAM ============================================ 1. Wyrzucilbym CO Aur. Ta gwiazda ma juz sporo obserwacji, nie jest wiec bardzo priorytetowa w porownaniu z innymi obiektami z listy. 2. Dla mnie oczywiscie najciekawsze sa klasyczne gwiazdy pulsujace. Moja lista priortetow bylaby nastepujaca: a) V473 Lyr b) RR Gem - ta gwiazda jest slaba a amplituda efektu Blazki dosc mala !! Moze byc trudno, ale warto sprobowac. c) V440 Per, Polaris 3. gwiazdy typu DCST o BCEP sa zapewne bardzo ciekawe dla Aloszy, ktory ma kody do szczegolowego modelowania ich pulsacji. Z tej grupy wybieralbym w pierwszej kolejnosci obiekty, dla ktorych sa wyznaczone czestosci z fotometrii. Majac Vr i fotometrie mozna zrobic identyfikacje modow i szanse na udana analize sejsmologiczna znacznie rosna. 4. Czy twoj spektrograf moze robic gwiazdy BCEP ? To jest zupelnie co innego niz cefeody i DSC (inna temperatura czyli ZUPELNIE inne widmo) 5. EA/DSCT: masz 4 takie gwiazdy na liscie. Jesli chcesz tylko wyznaczyc orbity, to OK. jesli chcesz rowniez mierzyc czestosci oscylacji, to chyba ogranicz sie do dwoch obiektow. Lepiej miec mniej gwiazd ale zrobionych solidniej. Sukces sejsmologii bardzo zalezy od ilosci wykrytych modow, a ta silnie zalezy od S/N. Potrzeba dyzo danych. Propozycja od JKA ================== beta Aur: praca Southworth i in. 2007(?) oparta na doskonalej fotometrii (WIRE) i spektroskopii z 1948r z bledem 1.5 km/s Podwojna zacmieniowa(czesciowa) P=3.96d o prawie rownych glebokosciach i silnym efekcie oswietlenia. WIRE-> Bruntt, H & Buzasi D.L., 2006 Mem Soc Astr It 77, 278