NOVAE WHERE SIMULATIONS MEET OBSERVATIONS YAEL HILLMAN AMNH

NOVAE, WHERE SIMULATIONS MEET OBSERVATIONS YAEL HILLMAN AMNH, NY, USA, & WEIZMANN INSTITUTE OF SCIENCE, ISRAEL VSS SYMPOSIUM 2018

OVERVIEW Novae - what are they and why do they happen? Nova light curve features How models help us understand observations Why we need long-term modeling

NOVAE

NOVAE C+O TNR nova flash

NOVAE – TYPICAL LIGHT CURVE Contracting radius Co ns Expanding radius ta nt ra di us st ar t acc. stage

NOVAE - MODELING Pressure, radius, mass, density, temperature, opacity, energy…

NOVAE - MODELING

NOVAE – CLASSICAL OR RECURRENT? A L L N O V A E A R E C U R R E N T definition observed(# of times) classical =1 >100 recurrent >1 <100

CONTENT BASED ON "Nova Multiwavelength Light Curves: Predicting UV Precursor Flashes and Pre-Max. Halts", Y. Hillman, D. Prialnik, A. Kovetz, M. M. Shara and J. D. Neill, MNRAS 437, 1962, 2014 "Observational Signatures of SNIa Progenitors, as Predicted by Models", Y. Hillman, D. Prialnik, A. Kovetz and M. M. Shara, MNRAS, 446, 1924, 2015 "Growing WDs to the Chandrasekhar Limit: The Parameter Space of the SD SNIa Channel", Y. Hillman, D. Prialnik, A. Kovetz and M. M. Shara, Ap. J, 819, 168, 2016 "Temporal resolution of a pre-max. halt in a CN: V 5589 Sgr observed with STEREO HI-1 B“, S. P. S. Eyres, D. Bewsher, Y. Hillman, et al. , MNRAS 467, 2684, 2017 "The Masses and Accretion Rates of White Dwarfs in Classical and Recurrent Novae”, M. M. Shara, and D. Prialnik, Y. Hillman, A. Kovetz, accepted for publication in Ap. J, 2018

CONTENT BASED ON "Comprehensive Photometric Histories of All Known Galactic Recurrent Novae", B. E. Schaefer, Ap. JS 187, 275, 2010 "Catalog of 93 Nova Light Curves: Classification and Properties“, R. J. Strope, B. E. Schaefer, A. A. Henden, AJ 140, 34, 2010 "An Extended Grid of Nova Models. II. The Parameter Space of Nova Outbursts“, O. Yaron, D. Prialnik, M. M. Shara, A. Kovetz, Ap. J, 623, 398, 2005

OVERVIEW Novae - what are they and why do they happen? Nova light curve features How models help us understand observations Why we need long-term modeling

FEATURES OF NOVA LIGHT CURVES OUTLINE Variance of nova light curves Pre-maximum flashes/halts Light curve decline classification

FEATURES OF NOVA LIGHT CURVES

FEATURES OF NOVA LIGHT CURVES Log(Teff[K]) Log(L[LSun]) Log(R[RSun])

FEATURES OF NOVA LIGHT CURVES Ma ss los s s rise T eftfag cline e & d L e d T eff & Rapi L w the Slo age nov st a n io t re c Ac

FEATURES OF NOVA LIGHT CURVES Ma ss los s s ri&se. T eff decline f. L ow eft age Sl. T & L d i p Ra the e g a nov st a n io t re c Ac

PRE-MAXIMUM UV FLASH Expected short UV flash prior to mass loss Found in some models (low mass WDs) convection receding from the photosphere

PRE-MAXIMUM UV FLASH - OBSERVATIONS …NOT just in models: M 31 2009 -10 b Observed in UV + VIS Cao et al. , 2012, Ap. J, 752, 133

PRE-MAXIMUM UV HALT - OBSERVATIONS Hounsell et al. , 2010, Ap. J, 724, 480

PRE-MAXIMUM VIS HALT - OBSERVATIONS Nova V 5589 Sgr Two pre-max halts: ~ 0. 5 mag STERE O Model ~1 hour -1. 1 -0. 95 -0. 8 -0. 65 -0. 35 -0. 2

MORE OF MODELS VS. OBSERVATIONS 500 day classification: th o o m S

at to Fl 500 day classification: p MORE OF MODELS VS. OBSERVATIONS

MORE OF MODELS VS. OBSERVATIONS ea at Pl u 500 day classification:

MORE OF MODELS VS. OBSERVATIONS Cu sp 500 day classification:

MORE OF MODELS VS. OBSERVATIONS 500 day classification: s a n tio O il sc

OVERVIEW Novae - what are they and why do they happen? Nova light curve features How models help us understand observations Why we need long-term modeling

COMBINING MODELS AND OBSERVATIONS

INPUT NOVA MODELS OUTPUT

OBSERVED NOT OBSERVED NOVA OBSERVATIONS Binary evolution SNIa progenitor

NOVA OBSERVATIONS - DATABASES

mag t[d]

CLASSICAL NOVAE

CLASSICAL NOVAE D OBSERVE So we get: For 82 CNe

RECURRENT NOVAE

RECURRENT NOVAE D OBSERVE So we get: For 10 RNe

MODELS MEET OBSERVATIONS NOVA BT Mon 1939 U Sco (RN) T Cr. B (RN) V 603 Aql 1918 CI Aql (RN) DQ Her 1934 MODEL 0. 95 1. 36 1. 32 1. 24 1. 21 0. 95 OBSERVATION REFERENCE Smith et al. (1998) Thoroughgood et al. (2001) Belczynski & Mikolajewska (1998) Arenas et al. (2000) Sahman et al. (2013) Robinson (1976) Hutchings et al. (1979) Horne et al. (1993)

NOVAE – DISTRIBUTIONS VIA OBSERVATIONS

NOVAE – TRUE VS. OBSERVED DISTRIBUTIONS BUT:

NOVAE – RECURRENCE PERIOD

Most probable to see Most probable to exist

RNe CNe SUMMARY