stars with large amplitudes Evgeni Semkov 1 , Stoyanka Peneva 1 , - PowerPoint PPT Presentation

Long term photometry of UXor stars with large amplitudes Evgeni Semkov 1 , Stoyanka Peneva 1 , Sunay Ibryamov 2 , Asen Mutafov 1 1 Institute of Astronomy and Natonal Astronomical Observatory, Bulgarian Academy of Sciences, Sofia, Bulgaria 2 Department of Physics and Astronomy, University of Shumen, Shumen, Bulgaria Second International Workshop “The UX Ori type stars and related topics” St. Petersburg, 30 September - 4 October 2019

V1184 Tau (CB 34 V) Discovered by Yun, Moreira, Alves, and Strom (1997) in the region of Bok globule CB 34. POSS1 POSS2

Spectral Observations of V1184 Tau Optical spectrum of V1184 Tau obtained on 24 March 2001.

I-light curve of V1184 Tau 2002 2004 2006 2008 2010 2012 2014 2016 2018 2020 12 13 14 15 I 16 17 18 52000 52500 53000 53500 54000 54500 55000 55500 56000 56500 57000 57500 58000 58500 JD

V1184 Tau 15.0 14.0 16.0 15.0 17.0 16.0 V R 18.0 17.0 19.0 18.0 20.0 19.0 2.0 2.2 2.4 2.6 2.8 3.0 3.2 3.4 3.6 3.8 0.8 1.0 1.2 1.4 1.6 1.8 2.0 V-I R-I Color indices V− I versus the stellar magnitude V and V − R versus R. The black diamonds denote observations from Oct. 2000 to Apr. 2003 (maximum level of brightness), the green diamonds observations from Aug. 2003 to Mar. 2010 (when the brightness of the star dropped) and the pink diamonds from Aug. 2010 to Apr. 2015. the star increased).

Long term B,R-light curves of V1184 Tau 1940 1950 1960 1970 1980 1990 2000 2010 2020 14 R B/pg 15 16 Magnitude 17 18 19 20 21 28000 32000 36000 40000 44000 48000 52000 56000 JD (24...)

V350 Cep Discovered by Gyulbudaghian & Sarkissian (1977) in the region of NGC 7129. Observed outburst 5 m in R POSS1 POSS2

V350 Cep

Optical spectrum of V350 Cep

UBVRI optical photometry of V350 Cep 1994 1996 1998 2000 2002 2004 2006 2008 2010 2012 2014 2016 2018 2020 13 14 15 Magnitudes 16 17 18 I R V 19 B U+1.5 20 49000 50000 51000 52000 53000 54000 55000 56000 57000 58000 59000 JD (24...)

V350 Cep 14 15 16 Magnitudes 17 18 I R 19 V B U+1.5 57300 57400 57500 57600 57700 JD (24...) UBVRI- -light curves of V350 Cep in the period August 2015 - November 2016

V350 Cep 15.5 15.5 15.5 16.0 16.0 16.0 16.5 16.5 16.5 V V V 17.0 17.0 17.0 17.5 17.5 17.5 18.0 18.0 18.0 1.6 2.0 2.4 2.8 0.4 0.8 1.2 1.6 0.8 1.2 1.6 V-I V-R B-V Color indices V−I, V−R, and B−V versus the stellar V magnitude of V350 Cep.

Long term B-light curve of V350 Cep 1955 1960 1965 1970 1975 1980 1985 1990 1995 2000 2005 2010 2015 2020 16 17 B/pg [mag] 18 19 20 21 35000 37500 40000 42500 45000 47500 50000 52500 55000 57500 JD (24...)

Star forming region Northern America/Pelican nebulae

V521 Cyg (LkH a 188) 1986 1989 1992 1995 1998 2001 2004 2007 2010 2013 2016 2019 11 I R+0.5 12 V+1.0 B+1.5 13 14 Magnitudes 15 16 17 18 19 46500 48000 49500 51000 52500 54000 55500 57000 58500 J.D. (24...) V521 Cyg was discovered and the star was classified as a RW Aurigae type by Hoffmeister 1949. Herbig & Bell 1988 classified it as T Tauri star with spectral type G8. Grankin et al. 2007 conduct the long-term photometric monitoring providing light curves of V521 Cyg from 1986 to 2003.

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stars with large amplitudes Evgeni Semkov 1 , Stoyanka Peneva 1 , - PowerPoint PPT Presentation

Long term photometry of UXor stars with large amplitudes Evgeni Semkov 1 , Stoyanka Peneva 1 , Sunay Ibryamov 2 , Asen Mutafov 1 1 Institute of Astronomy and Natonal Astronomical Observatory, Bulgarian Academy of Sciences, Sofia, Bulgaria 2

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stars with large amplitudes Evgeni Semkov 1 , Stoyanka Peneva 1 , - PowerPoint PPT Presentation

Long term photometry of UXor stars with large amplitudes Evgeni Semkov 1 , Stoyanka Peneva 1 , Sunay Ibryamov 2 , Asen Mutafov 1 1 Institute of Astronomy and Natonal Astronomical Observatory, Bulgarian Academy of Sciences, Sofia, Bulgaria 2

MHV amplitudes in N=4 SUSY Yang-Mills theory and quantum geometry of the momentum space Alexander

Coaction structure for Feynman amplitudes and a small graphs principle Francis Brown, IH

PULSAR TIMING ARRAYS SKY FULL OF STARS STARS SKY FULL OF STARS STARS Gravity versus

New geometric structures in scattering amplitudes The anatomy of

Integrable Deformations for N = 4 SYM and ABJM Amplitudes Till Bargheer IAS Princeton Dec 12,

for Scattering Amplitudes MHV @ 30, FermiLab 18.3.2016 Pierpaolo Mastrolia Physics and

Stars Stars Stars form from massive clouds of dust and gas in stellar nurseries. Stars Gravity

HC177: Biotech &amp; Art We used to think fate was in our stars. Now we know, in large

EFTs from the soft limits of scattering amplitudes Jaroslav Trnka Center for Quantum

THE EVALUATION OF STRING AMPLITUDES David B. Fairlie May 21, 2007 Abstract The geometrical

STARS Changes 2019-2020 PED STARS Team Richard Trujillo Deputy CIO Alecia Moll

Rota1on!and!convec1on!in!cool!MS!stars! ! On!the!MS:! ! Fully!convec1ve!stars!below!M &quot;

ON-SHELL METHODS FOR ONE-LOOP AMPLITUDES Darren Forde (SLAC) In collaboration with C. Berger, Z.

Signatures of first stars in and from dwarf galaxies Else Starkenburg First Stars, can we

The helicity amplitudes in the hypercentral Constituent Quark Model Mauro Giannini University of

The Pink Lecture Series: Scattering Amplitudes in String Theory Daniel H artl

Scattering amplitudes from the amplituhedron NMHV volume forms Andrea Orta

more-than-MHV amplitudes in QCD Simon Badger 18th March 2016 MHV@30, Fermilab, 16th-19th March

Tree-level scattering amplitudes in N = 4 SYM from integrability Tomek ukowski Mathematical

Superstring amplitudes with the pure spinor formalism Carlos R. Mafra STAG Research Centre and

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Stellar Nursery Stars gravitationally collapse from clouds of H and He Stars form from

Stellar Evolution: Low Mass Stars Mass 2-3 M sun But what about High Mass Stars and all of

Masses are much harder than Binary Stars to the Rescue!! distance, luminosity, or temperature

HC177: Biotech & Art We used to think fate was in our stars. Now we know, in large

Rota1on!and!convec1on!in!cool!MS!stars! ! On!the!MS:! ! Fully!convec1ve!stars!below!M "