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1 KT Eridani I8GM1/

2 Abstract KT Eridani(Nova Eridani 29) (UT) (R 4) (lter: B, V, y, Rc) He I, N II, N III Hα FWHM 34km/s He/N nova 148 (GSC ) ASAS Pi of the sky t 2 = 62 ± 3 t 3 = 143 ± 7 KT Eri very fast nova MMRD = 93 ± 7 M V r = 1 ± 3 kpc

3 1 (guest star) [1, 2, 3] 16 7 [4] 1572 (Tycho Brahe) 14 (nova stella) nova new (Harvard College Observatory) ( ) (K Lundmark) (B P Gerasimovic) 193 [5, 6] ashing nova slow nova (Dean B McLaughlin) [7] 2 t 2 3 t 3 fast, average, 1

4 slow, RT Ser *1 4 t (Cecilia Payne-Gaposchkin) very fast, fast, moderately fast, slow, very slow 5 [8] t (Hilmar W Duerbeck) fast (NA), slow (NB), extremely slow (NC) 3 [9] t 3 (GCVS; General Catalogue of Variable Stars) pre-nova 1942 [1, 11] [8] 199 (Robert E Williams) [12, 13] (permitted-line phase) (auroral-line phase) (coronal-line phase) (nebular-line phase) 4 ( ) He/N nova FeII nova (Merile F Walker) 1959 (Robert P Kraft) DQ Herculis(Nova Herculis 1934) [14, 15] DQ Her 4 39 ( day) DQ Her (close binary system) DQ Her *1 199 very slow nova 2

5 (accretion disk) (cataclysmic variable star) (classical nova) (recurrent nova) (dwarf nova) (nova-like variable) 4 (polar) (intermediate polar) [16] DQ Her ( ) (thermonuclear runaway) 197 (Summer Starreld) [17, 18]) CCD 1m CCD 2 3cm 26 Be ( 26 [19]) ( 27 [2]) Wolf-Rayet ( 28 [21]) 28 4 V2491 Cyg KT Eridani ( possible nova Eridani 29, KT Eri) VSOLJ-news 227 KT Eri 148 (GSC ) 3

6 KT Eri t 2, t 3 (B-V, V-R) KT Eridani

7 2 (cataclysmic variable) (white dwarf) ( G M) (close binary system) 1 1 (roche lobe) (Lagrangian point)l 1 ( ) (accretion disk) hot spot bright spot Fig 1 4 Fig 1: (Robinson 1976) 21 (classical nova) (6 19 ) ( 31, 32 ) 5

8 Table 1: W Liller( ) V2574 Oph Discovery date (year month day) Name Discoverer V5114 Sgr V1186 Sco ASAS-3( ) V1187 Sco V574 Pup V2361 Cyg V382 Nor W Liller( ) V378 Ser ASAS V5115 Sgr V5116 Sgr W Liller( ) V1188 Sco ASAS V147 Cen W Liller( ) V476 Sct V477 Sct ASAS V2575 Oph ASAS V5117 Sgr W Liller( ) V2362 Cyg V2576 Oph P Williams(! " ) V165 Cen W Liller( ) V128 Sco V1281 Sco V2467 Cyg V2615 Oph V5558 Sgr V39 Nor W Liller( ) V458 Vul #$%& V597 Pup AJS Pereira(' ( )( ) V459 Vul + * +,-/ V2468 Cyg * (24 28) [24] NR TrA N Brown( 12! " ) V2491 Cyg 12 & V5579 Sgr 12 & V267 Oph & V2671 Oph 12 & V139 Sco & V1721 Aql QY Mus W Liller( ) V679 Car Pi of the Sky( '!: ;<=">?@ ) V558 Sgr W Liller( ) (nova eruption) ( 34 ) 13M Hellier 21 [23]) M ( 6M M 13M 1 9 M /yrs 3 6M 6

9 5 1 Table 1 ASAS The All Sky Automated Survey 22 (recurrent nova) 2 ( ) 1 5 M /yrs Fig 2: RS Oph 54 (data from AAVSO) M 1958 RS Oph( RS) U Sco( U) Fig 2 AAVSO *2 RS Oph 54 RS Oph U Sco *3 ( ) RS Oph *2 The American Association of Variable Star Observers *3 U Sco Barbara G Harris 8 7 7

10 U Sco 123 Ia ( & 29 [25]) 23 (dwarf nova) (outburst) (disk instability) Fig 3: (Osaki 1974, 1996) [25] q Fig 3 2 Fig 4: U Gem 26 3 (data from AAVSO) 1 perid gap U Gem (SS Cyg) U Gem

3 1 Fig 4 26 3 U Gem 232 SU UMa SU UMa (normal -25 2873-2 outburst) (superoutburst) 2-15 -1-5 5 (superhump) 1 2 15 (Fig 5) mag 1 2 376 381 386 391 396 SU UMa Fig 5: SU UMa VY Aqr 28

11 3 1 Fig U Gem 232 SU UMa SU UMa (normal outburst) (superoutburst) (superhump) (Fig 5) mag SU UMa Fig 5: SU UMa VY Aqr ( K Imamura, N Kunitomi) Fig 5 WD Secondary disk UT 1 P prec = 1 P orb 1 P sh (1) P prec P orb P sh Fig 6 (P sh ) Fig 6: P orb P sh SU UMa WZ Sge ( 1 ) ER UMa ( 1 ) (SU UMa 1 1 ) 9

12 233 Z Cam Z Cam (mass transfer rate) (Fig 3) U Gem Fig 7 Z Cam U Gem standstill standstill Fig 7: Z Cam 23 (data from AAVSO) 24 (nova-like variable, NL ) Z Cam standstill 25 (post nova ) Fig 8 TT Ari Z Cam Fig 8: TT Ari 1977 (data (Fig 3) from AAVSO) 32 1

13 3 Payne-Gaposchkin (1957) Warner (1995) Hellier (21) Bode & Evans (28) Gray & Corbally (29) [8, 23, 26, 27, 28] Fig 9: (Payne-Gaposchkin 1957 [8]) Fig 9 pre nova initial rise pre-max halt nal rise early decline transition phase nal decline post nova transition phase 11

14 1K 2K ( 1µm 1µm) Fig 1 V1494 Aql Fig 1: V1494 Aql (Nova Aql 1992 No 2) [23] Data from AAVSO Fig 11 (V15 Cyg) (HR Del) Payne-Gaposchkin (1957) 2 ( ) t 2 5 [8] Duerbeck (1981) 3 ( ) t 3 3 [9] Table 2 Warner (1995) t 2 t 3 t 3 275t 88 2 (2) [26] Fig 11: V15 Cyg (Nova Cyg 1975) & HR Del (Nova Del 1967) [23] Data from AAVSO 12

15 Table 2: [8, 9] Author Speed class t 2 (days) t 3 (days) Payne-Gaposchkin Very fast < 1 Fast Moderately fast 26-8 Slow Very slow Duerbeck Fast (NA) < 1 Slow (NB) 1 Extremely slow (NC) ~ 1 year Kato & Hachisu (1994) [29] 312 (MMRD) Fig 12: MMRD t 2 [3] Fig 12 13

16 MMRD(Maximum Magnitude/Rate of Decline) 197 MMRD Downes & Duerbeck (2) t 2 M V,max = 1132(±44) + 255(±32) log t 2 (3) t 3 M V,max = 1199(±56) + 254(±35) log t 3 (4) [3] t 2 t 3 M V m V,max M V,max = 5 log r 1 pc + A V (5) m V V V A V (pre nova ) (post nova ) (permitted line) (fobidden line) Williams (199) 4 phase [12] P: (permitted line phase) A: (auroral line phase) C: (coronal line phase) N: (nebular line phase) (optically thick) OI, FeII, MgII, NII, OII ([OIII] ) 14

17 (optically thin) 1 Fig13 phase C P N A Fig 13: phase P Williams (199) [12] A C N Williams phase [31] CTIO (Cerro Tololo Inter-American Observatory) phase (P) ˆ he: He I λ5876, λ765 ˆ he + : He II λ4686 ˆ c: C IV λ585; C II λ7234 ˆ n: N II λ5679, λ51; N III λ464; N V λ465 ˆ fe: Fe II λ518, λ5169, λ5317 ˆ na: Na I λ

18 (A) : ˆ n: [N II] λ5755 ˆ o: [O I] λ5577; [O II] λ7325; [O III] λ4363 ˆ ne: [Ne III] λ3343; [Ne IV] λ4721 ˆ s: [S I] λ7725; [S III] λ6312 (C) ˆ a: [N II] λ5755; [O I] λ5577; [O II] λ7319, λ733; [O III] λ4363 ˆ he: He I λ5876, λ765 ˆ he + : He II λ4686 ˆ n: N II λ5679; N III λ464; [N II] λ6584 ˆ o: [O III] λ57 ˆ ne: [Ne III] λ3869; [Ne V] λ3426 ˆ fe: [Fe X] λ6375; [Fe XIV] λ533 (N) ˆ n: [N II] λ6584 ˆ o: [O I] λ63; [O III] λ57 ˆ ne: [Ne III] λ3869; [Ne V] λ3426 ˆ fe: [Fe II] λ4244, λ5159; [Fe III] λ4658, λ527; [Fe V] λ472; [Fe VI] λ5176; [Fe VII] λ687 P n Fig 14 Williams V416 Sgr (Nova Sgr 1991) 16

19 Fig 14: V416 Sgr (Nova Sgr 1991) [31] (8 1 ) (9 2 ) (1 1 ) 322 ( ) Fe II Na I, O I, Mg I, Ca II Fe II nova (Fig15) He N He/N nova (Fig16) [13] 17

20 Fig 15: Fe II nova [13] Fig 16: He/N nova [13] Fe II nova P Cygni He/N nova Williams (1992) [13] Fe II nova ( ) He/N nova ( ) 18

21 P Cygni (optically thin) (optically thick) Fig17 P Cygni P Cygni P Cyg( P ) optically thin optically thick observer Fig 17: P Cygni 33 (thermonuclear runaway) [17, 18] 2 19

22 (1cc 1t ) 2 ( 1 H) (e + ) ( 2 H) 3 ( 3 He) 4 ( 4 He) pp (proton-proton chain reaction) Fig 18 e + 1 H 1 H 1 H 2 H 3 He 1 H e + 1 H 4 He 1 H 2 H 3 He 1 H 1 H Fig 18: pp (proton-proton chain reaction) [32] ν γ 2

23 CNO (CNO cycle reaction) Fig 19 ( T 18 ) 4 He e + 15 N 1 H 12 C 1 H 15 O 13 N 1 H e + 14 N 1 H 13 C Fig 19: CNO (CNO cycle reaction) [32] 21

24 4 KT Eridani ( KT ) KT Eridani ( possible nova Eridani 29, KT Eri) VSOLJ-news 227 KT Eri : 4 h 47 m 54 s 21 1 d KT Eri N N Fig 2: V KT Eri 16' E E 1'7 KT Eri GSC *4 148 (GSC ) Pi of the sky ASAS AstroArts ( 5 KT Eri (VSOLJ; Variable Stars Observers League of Japan) Table *4 Guide Star Catalogue 22

25 Table 3: KT Eri ( ) ASAS Pi of the sky (VSOLJ) Obs Date (year/month/day [UT]) magnitude Color Observer 29/11/ R Pi of the sky 29/11/ R Pi of the sky 29/11/ R Pi of the sky 29/11/ R I Ootuki* 29/11/ V I Ootuki 29/11/ B I Ootuki 29/11/ R I Ootuki 29/11/ V I Ootuki 29/11/ B I Ootuki 29/11/ R Pi of the sky 29/11/ R Pi of the sky 29/11/ R Pi of the sky 29/11/ R A Kawamura** 29/11/ R A Kawamura 29/11/ V A Kawamura 29/11/ V A Kawamura 29/11/ B A Kawamura 29/11/ B A Kawamura 29/11/ R Pi of the sky 29/11/ R Pi of the sky 29/11/ V ASAS 29/11/ R Pi of the sky 29/11/ R Pi of the sky 29/11/ R Pi of the sky 29/11/ C Pi of the sky 29/11/ V ASAS 29/11/ C Pi of the sky 29/11/ C Pi of the sky 29/11/ V ASAS 29/11/ C Pi of the sky 29/11/ C Pi of the sky 29/11/ C Pi of the sky * Isao Ootuki (Miyagi, Japan), inst : EOS4D + 17mm (F4) ** Akira Kawamura (Gunma, Japan), inst : EOS5D mm (F35-45) 23

26 Table 4 Table 4: Celestron C11 Celestron C9 D=28cm, F1 D=235cm, F63 NJP Temma2 EM-2 Temma2 SBIG DSS-7 B, V, y, Rc CCD SBIG ST-42 CCD SBIG ST-7XE 511 DSS-7(DSS; Deep Space Spectrograph) SBIG (SBIG; Santa Barbara Instrument Group) DSS-7 (F ) F1 F1 ˆ : 15Å(R 4) : 54Å/1pixcel ˆ ˆ : Å ˆ : 5µ, 1µ, 2µ, 4µ 1 Fig 21 DSS-7 24

27 CCD DSS-7 CCD Fig 21: DSS-7 SBIG HP [33], DSS-7 4 Fig 22 5µ DSS-7 Fig 22: CCD (C11 + DSS-7 + ST-42) 25

28 CCD ST-42 DSS-7 SBIG CCD Kodak KAF-42ME ˆ CCD : 69 46mm : pics ˆ ˆ : 9 9µ ˆ : 16bit (65536 ) ˆ Full well capacity: 1, e ˆ : 1 ( ) CCD ( ) CCD ST-42 5, (Fig 23) 4, Count Exposure time (sec) Fig 23: CCD ST

29 512 CCD SBIG ST-7XE CCD Kodak KAF-41E ˆ CCD : 69 46mm : pics ˆ ˆ : 9 9µ ˆ : 16bit (65536 ) ˆ Full well capacity: 1, e ˆ : 1 ( ) CCD (24) 5, [34] 4, B, V, y, Rc 4 B, V, Rc, ( U, Ic ) Johnson-Cousins UBVRI system U (ultraviolet), B (blue), V (visual) 1953 Johnson Morgan [35] Rc (red), Ic (infrared) 198 Cousins [36] 25 Bessel CCD Table 5 Rc, Ic "c" Cousins u (ultraviolet), v (violet), b (blue), y (yellow) strömgren uvby sytem 196 Strömgren Bessel CCD Fig 24 strömgren y 25 27

30 Table 5: [37] ( ) ( ) U B V Rc Ic u v b y Fig 24: Johnson-Cousins UBVRI system ( ) strömgren uvby sytem ( ) [38] (Å) (KT Eri) ( ) (Fig 25) DSS *5 (C) *5 Digitized Sky Survey Space Telescope Science Institute (STScI) 28

があるこれは後に差測光を行う時に使用するためである (詳しくは 64 章) 本研究では Tycho 2 星表*6 を参照し比較星として TYC532515441 (B =

画像中央の星が目的星 (KT Eri) 加えて測光時に使用した比較星 (C) も示す Data from DSS 522 CCD カメラの冷却観測開始前には CCD

一般に CCD チップを冷却することでダークノイズを抑えることができる液体窒素を用いれば 7 まで冷却が可能で CCD のダークノイズは皆無に等しくなると言われている

さらに冷却が安定するまで数時間を要しそのため観測開始の数時間前から冷却を開始する必要があるペルチェ素子とは電気を流すことで片面が冷え反対側の面は熱くなるという性質を

31 があるこれは後に差測光を行う時に使用するためである (詳しくは 64 章) 本研究では Tycho 2 星表*6 を参照し比較星として TYC (B = 181, V = 124, R = 995, B V = 57) を選んだ (C) (KT Eri) N E Fig 25: ファインディングチャート視野角は 3' 3' 画像中央の星が目的星 (KT Eri) 加えて測光時に使用した比較星 (C) も示す Data from DSS 522 CCD カメラの冷却観測開始前には CCD カメラを冷却する必要がある CCD は装置の電源を入れた時点で熱的に発生する暗電流が各ピクセルに少しずつ溜まる性質があるこれをダークノイズと呼びその量は温度に強く依存し一般に CCD チップを冷却することでダークノイズを抑えることができる液体窒素を用いれば 7 まで冷却が可能で CCD のダークノイズは皆無に等しくなると言われているしかし本研究で用いた冷却 CCD カメラの冷却方式はペルチェ素子による一段電子冷却でありスペック上外気温から 25 まで冷却可能となっているさらに冷却が安定するまで数時間を要しそのため観測開始の数時間前から冷却を開始する必要があるペルチェ素子とは電気を流すことで片面が冷え反対側の面は熱くなるという性質を持った半導体であるペルチェ素子で低温を作り出すには放熱側の熱を逃がす必要があ *6 Hipparcos 衛星が観測した位置星表前身である Tycho 星表の改訂版であり限界等級約 11 等約 25 万個の恒星について記載されている 29

32 CCD Telescope Tracer 2 1 Telescope Tracer 2 RS232C Telescope Tracer 2 2 ( 1 ) 3 ( ) CCD (5mm, F28) ( 96, 7 ) 3 CCD Telescope Tracer 2 4 SBIG CCDOPS 3

33 Table 6 Table 7 Table 6: Date Number of frames Cooling temp year month day (UT) Observer* a, c a, c a a, c a, b, c a, c a a, c a, c b, c a, c a, b, c a, b, c c a, c a, b, c a, b a, c a, b, c c a, b a, b a, b a, c a, b, c b, c a, b, c c a, c c a, b a, c b, c a * a: Kazuyoshi Imamura, b: Nanae Kunitomi, c: Mikiha Nose 31

34 Table 7: Date Number of frames year month day (UT) Filter Cooling temp Observer* B, V, y, Rc -1 a, c B, V, y, Rc -1 a, c B, V, y, Rc -1 a B, V, y, Rc -1 a, c B, V, y, Rc -1 a, b, c B, V, y, Rc -1 a, c B, V, y, Rc -1 a B, V, y, Rc -1 a, b, c B, V, y, Rc -1 a, c B, V, y, Rc -1 b, c B, V, y, Rc -1 a, c B, V, y, Rc -1 a, b, c B, V, y, Rc -1 a, b, c B, V, y, Rc -15 a, b, c B, V, y, Rc -15 c B, V, y, Rc -15 a, c B, V, y, Rc -15 a, b, c B, V, y, Rc -15 a, b Rc -15 c B, V, y, Rc -15 b, c B, V, y, Rc -15 a, c B, V, y, Rc -15 a, b, c B, V, y, Rc -15 c B, V, y, Rc -15 a, b B, V, y, Rc -15 a, b V, Rc -15 a, b B, V, y, Rc -15 a, c B, V, y, Rc -15 a, b, c B, V, y, Rc -15 b, c B, V, y, Rc -15 a, b, c B, V, y, Rc -15 a, c B, V, y, Rc -15 c B, V, y, Rc -15 a, b B, V, y, Rc -15 c B, V, y, Rc -15 a, c B, V, y, Rc -15 b, c B, V, y, Rc -15 a B, V, y, Rc -15 a * a: Kazuyoshi Imamura, b: Nanae Kunitomi, c: Mikiha Nose 32

35 6 BeSpec( : ) AIP4Win ver2 ( : Berry & Burnell 25) [39, 4] CCD (Fig 26) CCD Fig 26: 612 CCD CCD Fig 27: (Fig 27) 33

36 SN SN n n n 1/ n 1 16bit (1 ) (Fig 28 y ) pixcel Fig 29 pixcel 34

37 Fig 3 pixcel y x pixcel Fig 28: y pixcel number Fig 29: 35

38 14 Hg Hg 9 Hg 4 [O Hg ] Fig 3: Fig 31 ( ) x (Fig 28 x ) pixcel number pixcel number Fig 31: (1 ) 36

39 632 1 pixcel number (Å) Edomond Fig 32 DSS-7 Hydrogen (H ) (H ) (H ) Helium Fig 32: [41] ( ) ( ) (Å) 9 pixcel number λ = 286(±21) 1 4 n (±6)n + 835(±1) (6) (Fig 33) λ (Å) n pixcel number Å 37

40 pixcel number Fig 33: 9 64 aperture photometry ( ) Fig 34 3 (aperture) Fig 35 1 P star N 2 3 P sky N N pixcel 2 (L 1, L 2 ) (m 1, m 2 ) (7) m 1 m 2 = 25 log( L 2 L 1 ) (7) m 1 = 25 log L log L 2 + m 2 (8) m 1 = 25 log L 1 + Z (9) Z P star N P sky N t P star N = (L star + L sky ) t (1) P sky N = L sky t (11) L star = ( P star P sky ) N t = L 1 (12) 38

41 (9) m 1 = 25 log ( P star P sky ) N t + Z (13) aperture photometry Fig 34: AIP4Win ver2 aperture photometry P star N P sky N Fig 35: aperture photometry (V) (C) aperture photometry 2 *7 *7 (dierential photometry) V-C 39

42 N III Fig He I, N II, N III Williams (1992) Moore (1945) [13, 42] Appendix Exp time : 6s 5 H H N II 51, He I 516 N II 5679 He I 5876 KT Eri (UT: 29/11/26639) FWHM of H : 34 km/s H He I wavelength( ) Fig 36: (UT) (Å) 6 5 Fig 37 Hα (km/s) (v) (FWHM; Full Width at Half Maximum) v = λ λ c (14) λ λ c (3 1 5 km/s) DSS-7 15Å 7 km/s Fig 71 Hα FWHM km/s km/s km/s km/s 4

43 FWHM of H (km/s) /11/26 12/8 21/1/ JD [-24551] Fig 37: Hα FWHM (km/s) (JD) 1/ velocity (km/s) Fig 38: Hα (km/s) intensity 1 N III (464) He II (4648) Fig 38 1 NIII (464) HeII (4688) 29/11/ / /22 21/1/3 2 21/1/ Fig 39: N III (464) He II (4688) intensity 1 41

44 72 Fig 4 B, V, R, y Fig 41 (B-V, V-R; color index) Fig 42 y B-R magnitude JD [-24551] B V R y Fig 4: KT Eri B-V V-R JD [-24551] Fig 41: B-V( ) V-R( ) color index B-y y-r y-v B-R JD [-24551] Fig 42: (y-b, y-r, y-v, B-R) 42

45 KT Eri Hα FWHM km/s Hα FWHM N III (464) He II (4688) FWHM N III (464) N III (464) He II (4688) 1 13 He II (4688) Williams (1992) He/N nova t 2 t 3 Fig 45 ASAS t Pi of the sky VSOLJ KT Eri t (Fig 46) R t = ± 2 (JD) t 2 t 3 t 2 = 62 ± 3 (day), t 3 = 143 ± 7 (day) 43

46 KT Eri Payne-Gaposchkin(1957) very fat nova (t 2 :< 1day) Duerbeck (1981) fast (NA; t 3 < 1 day) magunitude B (VSOLJ) V (VSOLJ) R (Pi of the sky) C (Pi of the sky) B (OUS) Rc (OUS) V (OUS) y (OUS) R (VSOLJ) V (ASAS) JD [-24551] Fig 43: magnitude JD [-24551] Fig 44: t B V V R ( ) [43] 44

47 B V ( ) V Hα Hα B V 31 (t 2 ) (M V ) (3) KT Eri (M V,max ) M V,max = 93 ± 7 mag (m V,max = 55 mag) 31 (5) KT Eri (r) r = 1 ± 3 kpc (A V ) 83 ˆ He/N nova ˆ V 55 mag 9 mag ˆ t 2 = 62 ± 3 day (very fast nova) t 3 = 143 ± 7 day (NA) ˆ t 2 93 ± 7 mag 1 ± 3 kpc 21 1 KT Eri transition phase phase transition phase Appendix KT Eri V

48 15 KT Eri (A V ) KT Eri ( : 32d 12m 8s)

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52 Appendix 1 29/11/28 21/1/ Fig 45: (UT) Fig 46: (UT) Fig 47: (UT) 6 5 Fig 48: (UT) Fig 49: (UT) Fig 5: (UT) 6 5 5

53 relative inyensity Fig 51: (UT) 6 5 Fig 52: (UT) Fig 53: (UT) 6 5 Fig 54: (UT) Fig 55: (UT) Fig 56: (UT)

54 Fig 57: (UT) 6 1 Fig 58: (UT) relarive intensity wavelength( ) Fig 59: (UT) 6 1 Fig 6: (UT) wavelength( ) Fig 61: (UT) 6 7 Fig 62: (UT)

55 Fig 63: (UT) Fig 64: (UT) Fig 65: (UT) 6 1 Fig 66: (UT) Fig 67: (UT) 6 5 Fig 68: (UT)

56 Fig 69: (UT) 6 1 Fig 7: (UT) Fig 71: (UT) 6 7 Fig 72: (UT) Fig 73: (UT) 6 7 Fig 74: (UT)

57 Fig 75: (UT) Fig 76: (UT) Fig 77: (UT)

58 Appendix 2 Fig Fig 79 relative magnitude HJD-2455 Fig 78:

59 -18 29/12/ /1/12 relative magnitude relative magnitude relative magnitude HJD [-2455] /1/ HJD [-2455] HJD [-2455] /1/ HJD [-2455] /1/ relative magnitude /1/ HJD [-2455] HJD [-2455] Fig 79: 57

214 1 11 SU UMa AY Lyr AY ASASSN-14jv CCD ASASSN-14jv SU UMa WZ Sge 28 29 AY Lyr O-C

AY Lyr ASASSN-14jv CCD I11G22 214 1 11 SU UMa AY Lyr AY ASASSN-14jv CCD ASASSN-14jv SU UMa WZ Sge 28 29 AY Lyr O-C 1 4 1.1............................. 4 1.2................................ 5 2 7 3 9 4