V1280 Sco 2007 #1

Novae & Luminous Although the basics of the nova outburst are believed to be understood there remain many Transients specifics that are not. In recent years new luminous transients have been discovered that do not Jupiter fit into either the normal nova or supernova classificaon, including some that are observed only in the infrared. I will review recent developments and suggest a Robert Williams Nova Scorpii 2007 Space Telescope Science Institute model that explains the simultaneous presence of both dust and hard X-ray emission in novae.

Pacific Rim Conference Dec 2015 Thanks and best wishes to Sun KWOK Light Curves

Novae: Discovery & Nova Vel 1999 Light Curves d t3=9 [fast]

Nova Sco 2004 #1

d t3=75 [slow]

AAVSO GK Per (log)

GK Per/1901 T Pyx (+95 yrs) 1890/1902/1920/1944/1966/2011 (+?? yrs)

DQ Herculis/1934 (+45 yrs)

HR Del/1967 (+35 yr) IntermedPolarDiag

γ 8 Pαρ TNR (TFermi=10 K)

H (+He)

(C/O) Prototype Nova System (with magnetic field) Arp M31 MMRD

M31 Novae: Luminosity vs. Rate of Decline 11 11

−11 −11 −11 −11

−10.5 −10.5 −10.5 −10.5

−10 −10 −10 −10 ‘MMRD’−9.5 Relation −9.5 −9.5 −9.5

Mag −9 Mag −9 − − Mag −9 Mag −9 − − −8.5 −8.5 −8.5 −8.5 Novae Novae −8 Novae −8 Novae −8 −8

Absolute g −7.5 Absolute g −7.5 Absolute g −7.5 Absolute g −7.5

−7 −7 −7 −7

−6.5 −6.5 −6.5 −6.5

−6 −6 0 1 2 0 1 2 10 −6 10 10 10 −6 10 10 0 1 2 0 1 2 Timescale "t1" 10[day] 10 10 Timescale "t1" 10[day] 10 10 Timescale "t1" [day] Timescale "t1" [day] Fig. 11.— Maximum magnitude (absolute g-band) versus Fig. 13.— Comparison of the P60-FasTING nova sample rate of decline (time to decayFig. 11.— from peakMaximum by 1 mag). magnitude Gray re-(absolute(greeng-band) symbols) versus with theFig. Galactic 13.— recurrentComparison novae of the(blue P60-FasTING cir- nova sample gion denotes the dellarate Valle of & decline Livio (1995)(time to MMRD decay from relation peak bycles, 1 mag). data Gray from re- Schaefer(green (2009)). symbols) with the Galactic recurrent novae (blue cir- and dark gray dots thegion nova denotes sample the they della used. Valle The & Livio P60- (1995) MMRD relation cles, data from Schaefer (2009)). FasTING sample is shownand with dark symbols gray dots that the denote nova spectral sample they used. The P60- type — Fe II class (star),FasTING He/N classsample (circle), is shown spectrum with symbols with that denote spectral no prominent features fortype classification — Fe II class (squares) (star), and He/N no class spec- (circle), spectrum with no prominent features for classification (squares) and−11 no spec- trum (empty square). −11 trum (empty square). −10.5 −10.5

Arp, H. 1956, AJ,−10 61, 15 −10

−11 −9.5 −11 −9.5

−10.5 Mag −9 − −10.5 Mag −9 − −10 −8.5 −8.5 −10 Novae −9.5 −8 Novae −9.5 −8

Absolute g −7.5 Mag −9 Absolute g

− −7.5 Mag −9 − −8.5 −7 −7 Novae−8.5 −8 Novae −6.5 −8 −6.5

Absolute g −6 −7.5 0 1 2 Absolute g 10 −6 10 10 −7.5 0 1 2 Timescale "t1" 10[day] 10 10 −7 Timescale "t1" [day] −7 −6.5 Fig. 14.— Theoretical results of Yaron et al. (2005) over a −6.5 wide range of nova parametersFig. 14.— —Theoretical we use the results colors of of Yaron an et al. (2005) over a −6 0 1 2 wide range of nova parameters — we use the colors of an 10 10−6 10 A5V star to convert L4max to Mg and approximate t1 as 0 1 2 Timescale10 "t2" [day] 10 10 A5V star to convert L4max to Mg and approximate t1 as Timescale "t2" [day] tml/3. The size of the symbol is proportional to the mass of the white dwarf. Thet colorml/3. of The the size symbol of the denotes symbol tempera- is proportional to the mass of Fig. 12.— Maximum magnitude (absolute g−band) versus ture — 10 million K (red),the white 30 million dwarf. K The (green), color 50 of millionthe symbol denotes tempera- Fig. 12.— Maximum magnitude (absolute g−band) versus rate of decline (time to decay from peak by 2 mag). Only the K(blue).Emptycirclesdenoteloweraccretionrateintheture — 10 million K (red), 30 million K (green), 50 million six novae with the bestrate sampled of decline light (time curves to are decay shown. from peak by 2 mag). Only−12.3 the −10 K(blue).Emptycirclesdenoteloweraccretionrateinthe−1 range 10 —10 M⊙yr and−12. filled3 circles−10 denote−1 higher six novae with the best sampled light curves are shown. range 10−9 —10−6 M⊙−1yr and filled circles denote higher accretion rate in the range 10 —10 M⊙yr .Notethat−9 −6 −1 the density of circles isaccretion unrelated rate to the in relativethe range populati 10 —10ons. M⊙yr .Notethat the density of circles is unrelated to the relative populations. sten and O. Yaron for valuable feedback. We are grate- ful to A. Becker forsten making and his O. software Yaron forhotpants valuableand feedback. We are grate- wcsremap available forful public to A. use. Becker MMK for thanks making the his Gor- software hotpants and don and Betty Moorewcsremap Foundationavailable for the for publicHale Fellow- use. MMKas thanks a scientific the Gor- partnership among the California Insti- ship in support of graduatedon and study. Betty Moore S.B.C. Foundation is grateful for thetute Hale of Technology, Fellow- theas Universitya scientific of partnership California and among the the California Insti- for generous supportship from in Gary support and of Cynthia graduate Bengier, study. S.B.C.National is grateful Aeronauticstute and of Space Technology, Administration. the University The of California and the the Richard and Rhodafor generous Goldman support Fund, and from National Gary and CynthiaObservatory Bengier, was madeNational possible Aeronautics by the generous and Space finan- Administration. The Science Foundation (NSF)the Richard grant and AST0908886. Rhoda Goldman MMK Fund,cial and support National of the W.M.Observatory Keck Foundation. was made The possible authors by the generous finan- thanks the PalomarScience Observatory Foundation staff for (NSF) their helpgrant in AST0908886.wish to recognize MMK andcial acknowledge support of the the W.M. very significant Keck Foundation. The authors maximizing the efficiencythanks and the image Palomar quality Observatory of the Palo- staff forcultural their help role and in reverencewish to that recognize the summit and acknowledge of Mauna the very significant mar 60-inch. Some ofmaximizing the data presented the efficiency herein and were image ob- qualityKea of has the always Palo- had withincultural the role indigenous and reverence Hawaiian that com- the summit of Mauna tained at the W.M. Keckmar Observatory,60-inch. Some which of the is data operated presentedmunity. herein were We ob-are mostKea fortunate has always to have had the within opportunity the indigenous Hawaiian com- tained at the W.M. Keck Observatory, which is operated munity. We are most fortunate to have the opportunity Arp M31 MMRD

M31 Novae: Luminosity vs. Rate of Decline 11 11

−11 −11 −11 Kasliwal, M. et al. 2010, ApJL, 723, L98 −11 −10.5 (Palomar Transient Factory [PTF]) −10.5 −10.5 −10.5

−10 −10 −10 −10

−9.5 −9.5 −9.5 −9.5

Mag −9 Mag −9 − − Mag −9 Mag −9 − − −8.5 −8.5 −8.5 −8.5 Novae Novae −8 Novae −8 Novae −8 −8

Absolute g −7.5 Absolute g −7.5 Absolute g −7.5 Absolute g −7.5

−7 −7 −7 −7

−6.5 −6.5 −6.5 −6.5

−6 −6 0 1 2 0 1 2 −6 10 10 10 −6 10 10 10 0 1 2 0 1 2 10 Timescale "t1" 10[day] 10 10 Timescale "t1" 10[day] 10 Timescale "t1" [day] Timescale "t1" [day]

Henze et al.2008, A&A, 477, 67 Fig. 11.— Maximum magnitude (absolute g-band) versus Fig. 13.— Comparison of the P60-FasTING nova sample rate ofFig. decline 11.— (timeMaximum to decay magnitude from peak (absolute by 1 mag).g-band) Gray versus re- (greenFig. symbols) 13.— Comparison with the Galactic of the recurrent P60-FasTING novae nova(blue sample cir- gionrate denotes of decline the della (time Valle to decay & Livio from (1995) peak by MMRD 1 mag). relation Gray re- cles,(green data fromsymbols) Schaefer with (2009)). the Galactic recurrent novae (blue cir- andgion dark denotes gray dots the dellathe nova Valle sample & Livio they (1995) used. MMRD The P60- relation cles, data from Schaefer (2009)). FasTINGand dark sample gray is dots shown the with nova symbols sample that they denote used. spectral The P60- typeFasTING — Fe II sample class (star), is shown He/N with class symbols (circle), that spectrum denote spectralwith no prominenttype — Fe features II class for(star), classification He/N class (squares) (circle), and spectrum no spec- with no prominent features for classification (squares) and no spec- −11 trum (empty square). −11 trum (empty square). −10.5 −10.5

−10 −10

−11 −9.5 −11 −9.5

−10.5 Mag −9 − −10.5 Mag −9 − −10 −8.5 −8.5 −10 Novae −9.5 −8 Novae −9.5 −8

Absolute g −7.5 Mag −9 Absolute g

− −7.5 Mag −9 − −8.5 −7 −7 −8.5 Novae −8 Novae −6.5 −8 −6.5

Absolute g −6 −7.5 0 1 2 Absolute g −6 10 10 10 −7.5 0 1 2 10 Timescale "t1" 10[day] 10 −7 Timescale "t1" [day] −7 −6.5 Fig. 14.— Theoretical results of Yaron et al. (2005) over a −6.5 wideFig. range 14.— of novaTheoretical parameters results — of we Yaron use the et al. colors (2005) of over an a −6 0 1 2 wide range of nova parameters — we use the colors of an 10 −6 10 10 A5V star to convert L4max to Mg and approximate t1 as 0 1 2 10 Timescale 10"t2" [day] 10 A5V star to convert L4max to Mg and approximate t1 as Timescale "t2" [day] tml/3. The size of the symbol is proportional to the mass of thet whiteml/3. dwarf.The size The of the color symbol of the is symbol proportional denotes to tempera- the mass of Fig. 12.— Maximum magnitude (absolute g−band) versus turethe — white 10 million dwarf. K The (red), color 30 million of the symbol K (green), denotes 50 million tempera- Fig. 12.— Maximum magnitude (absolute g−band) versus rate of decline (time to decay from peak by 2 mag). Only the K(blue).Emptycirclesdenoteloweraccretionrateintheture — 10 million K (red), 30 million K (green), 50 million sixrate novae of with decline the (time best tosampled decay lightfrom curvespeak by are 2 mag). shown. Only the K(blue).Emptycirclesdenoteloweraccretionrateinthe−12.3 −10 −1 range 10 −12—10.3 −M10⊙yr and−1 filled circles denote higher six novae with the best sampled light curves are shown. range 10 —10 M⊙yr −9 and− filled6 circles−1 denote higher accretion rate in the range 10 —10−9 M−⊙6 yr .Notethat−1 theaccretion density of rate circles in theis unrelated range 10 to the—10 relativeM⊙yr populati.Notethatons. the density of circles is unrelated to the relative populations. sten and O. Yaron for valuable feedback. We are grate- fulsten to A. and Becker O. Yaron for making for valuable his software feedback.hotpants We areand grate- wcsremapful to A.available Becker for for public making use. his MMK software thankshotpants the Gor-and donwcsremap and Bettyavailable Moore for Foundation public use. for MMK the Halethanks Fellow- the Gor- as a scientific partnership among the California Insti- shipdon in and support Betty of Moore graduate Foundation study. S.B.C. for the is Hale grateful Fellow- tuteas of a Technology, scientific partnership the University among of California the California and the Insti- forship generous in support support of from graduate Gary study. and Cynthia S.B.C. Bengier, is grateful Nationaltute of Aeronautics Technology, and the University Space Administration. of California and The the thefor Richard generous and support Rhoda from Goldman Gary Fund, and Cynthia and National Bengier, ObservatoryNational Aeronautics was made possible and Space by the Administration. generous finan- The Sciencethe Richard Foundation and (NSF)Rhoda grant Goldman AST0908886. Fund, and MMK National cialObservatory support of the was W.M. made Keck possible Foundation. by the generous The authors finan- thanksScience the Foundation Palomar Observatory (NSF) grant staff AST0908886.for their help MMK in wishcial to support recognize of the and W.M. acknowledge Keck Foundation. the very significant The authors maximizingthanks the the Palomar efficiency Observatory and image quality staff for of their the Palo- help in culturalwish to role recognize and reverence and acknowledge that the summit the very of significant Mauna marmaximizing 60-inch. Some the e offfi theciency data and presented image quality herein of were the ob- Palo- Keacultural has always role had and within reverence the indigenous that the summit Hawaiian of com- Mauna tainedmar at 60-inch. the W.M. Some Keck of the Observatory, data presented which herein is operated were ob- munity.Kea has We always are most had fortunate within the to indigenous have the opportunity Hawaiian com- tained at the W.M. Keck Observatory, which is operated munity. We are most fortunate to have the opportunity ‘Nova’ V1309 Sco/08

?

V838 Mon

Mason+ 2010, A&A, 516, 108 ‘Nova’ V1309 Sco/08

?

V838 Mon

Mason+ 2010, A&A, 516, 108

4 Tylenda et al.: V1309 Sco OGLE-III corresponding to the 0.7 day period deacreases and in epoch 7 it practically disappears. 2002

5.2. Interpretation In principle one can consider three possible interpretations of the observed light variability, i.e. stellar pulsation, singlestarrota- tion, and eclipsing binary system.

5.2.1. Pulsation The light curve in early epochs may imply a stellar pulsation with a period of ∼0.7 day and an amplitude of ∼0.15 magnitude. This interpretation, however, encounters severe problems when explaining the observed evolution of V1309 Sco. As we show below, the progenitor was probably a K-type star. There is no class of pulsating stars, which could be reconciled with these characteristics, i.e a K-type star pulsating with the above period and amplitude. Moreover, to explain the observed evolution of the light curve displayed in Fig. 3, one would have to postulate aswitchofthestarpulsationtoaperiodexactlytwicelongeron atimescaleofafewyears,togetherwithagradualshortening of the period. This would be very difficult, if not impossible, to be understood within the present theory of stellar pulsation. Finally, there is no physical mechanism involving or resulting from a pulsation instability, which could explain the powerful 2008 eruption, when the object brightened by a factor of 104.

5.2.2. Rotation of a single star The observed light curve could have been explained by a sin- gle K-type star rotating with a period of ∼1.4 day and having two spots (or rather two groups of spots) on its surface in early epochs. The two spots would be replaced by one spot in epoch 7. The object would thus belong to the FK Com class of rapidly rotating giants (e.g. Bopp & Stencel 1981). There are, however, several differences between the progenitor of V1309 Sco and the FK Com stars. The 1.4 day period is short as for the FK Com stars. The very good phase stability of the observed light curve, seen in Fig. 3, implies that the spot(s) would have had to keep the same position(s) on the star surface over a time span of a few years. This seems to be very improbable given differential rota- tion and meridional circulation expected to be substantial in the case of a rapidly rotating star. Indeed, in the case of the FK Com stars, the spots are observed to migrate and change their posi- tion on much shorter time scales (Korhonen et al. 2007). Also Fig. 3. The light curves obtained from folding the data with the the systematic decrease of the rotational period is difficult to ex- period described by Eq. (1). Upper part: epochs 2 – 6. Lower plain in the case of a single star, and is not observed in the FK part: epoch 7 devided into five subsamples (time goes from a to Com stars. Finally, no eruption, as that of V1309 Sco in 2008, e). The zero point of the magnitude (ordinate) scale is arbitrary. was observed for the FK Com stars. In fact, there is no known mechanism, which could produce such a huge eruption in the 2008 case of a single giant, even if it is fast rotating. equally spaced in the phase and, in the early epochs, have sim- ilar shapes. This is the reason why the periodograms for these 5.2.3. A contact binary evolving to its merger epochs (see Appendix A) show a strong peak at a frequency twice greater (period twice shorter) than the main peak. In other We arethusleft with aneclipsingbinarysystem.As we showbe- words, the observations could have been interpreted with a pe- low, this possibility allows us to explain all the principal charac- riod of ∼0.7 day and a light curve with one maximum and min- teristics of the observed evolution of the V1309 Sco progenitor, imum. The periodograms however show, already from epoch 2, as well as the 2008 outburst. that the period twice longer (∼1.4 day) better reproduces the ob- The shape of the light curve, especially in early epochs servations. The reason is seen in the later epochs, when the first (two rounded maxima of comparable brightness and two equally maximum (at phase 0.25 in Fig. 3) in the light curve becomes spaced minima), implies that the progenitor of V1309 Sco was increasingly stronger than the second one. As a result the peak acontactbinary.Theorbitalperiodof∼1.4 day does not allow

Tylenda+ 2011, A&A, 528, 114 ……………. Merger of contact binary! Arp MMRD CastorMcCBubble

−24 45 Luminous Supernovae 10 Transients SCP06F6 SN2005ap SN2008es PTF09cnd −22 (PTF) SN2006gy PTF09cwl PTF09atu 44 PTF10cwr 10 SN2007bi PTF searched nearby galaxies for −20 transients. Dists known, so Mv Thermonuclear Supernovae 43 derived. Many intermediate ‘gap’ SN2002bj 10 ] V

−18 ]

= ‘intermed lum’ transients. 1 − Defined by their spectra, not PTF10bhp Core−Collapse Supernovae 42 PTF11bij 10 decay me. −16 .Ia Explosions PTF09dav PTF10iuv SN2005E

SN2008ha −14 41 Ca−rich SN2008S 10 Transients PTF10acbp Peak Luminosity [erg s NGC300OT Peak Luminosity [M −12 PTF10fqs Luminous 40 Red 10 V1309 Sco Novae −10 P60−M82OT−081119 M85 OT V838 Mon Classical Novae 39 M31 RV 10 −8 P60−M81OT−071213 Arp MMRD 38 −6 10 0 1 2 10 10 10 Kasliwal, M. et al. 2010, ApJL, 723, L98 Characteristic Timescale [day] Kasliwal, M. 2011, BASI, 39, 375

Luminosity

Transients Properties TransientsProperties

.

Optical Extinction & IR

QV Vul Dust Abs Nova QV Vul/87 Emission: Dust Formation

Visible IR

Gehrz et al. 1992, ApJ, 400, 671 Optical Extinction & IR

QV Vul Dust Abs Nova QV Vul/87 Emission: Dust Formation

Visible IR 1988ARA&A..26..377G

Gehrz, R. 1988, ARAA, 26, 377 Gehrz et al. 1992, ApJ, 400, 671 SPIRITS Program (M. Kasliwal, PI)

• Spitzer-warm Cycles 10 & 11: 338 + 790 hrs • L & M bands (3.6μ & 4.5μ) • ~200 galaxies d < 20 Mpc • Observing Cadence: 1,2,3 week/month/3-6 months

• Liming IR detecon: (m3.6<20 ; m4.5< 19) - d< 5 Mpc: MIR < -8.5 (novae) - d< 20 Mpc: MIR < -11.5 (explosive transients)

• Follow-up photometry & spectroscopy M101 Spitzer 3.6µ images SPIRITS has detected (Spitzer C10): Ø 21 SNe Ø 4 novae Ø 15 ‘gap’ transients (in spirals; no opcal counterparts) Ø 1200 IR variables MIR≈ -12.4

MIR≈ -11

MIR≈ -12