arXiv:astro-ph/9909159v1 9 Sep 1999 C htmtyadnwmdl f5mnrplanets minor 5 of Kiss models L.L. new and photometry CCD D nei 93 ea ta.19,Sa´ ta.1999). collisional al. possible Szab´o et detect 1994, to is al. aspect et longitudes important Detal Another different 1993, very Angelis at of (De obtained lightcurves coverage fainter multi-opposition phase on much full based study methods are to photometric modelling The of possible previously. the become than long- planets of has and minor advent it precision the era high With CCD rotation observations. requires the photometric planets and term minor shape the the of of modelling Ground-based Introduction 1. 1 2 Abstract. 3 agtbihns.Teotie ioi eid n am- and 4 – periods Lanzia sinodic 683 plitudes: obtained The the on brightness. mainly target depending be- ac- mag, achieved out 0.01–0.03 The between carried is 1999. curacy January, asteroids and faint 1998 moderately October, tween and faint 5 of 1 e words: (1990). Key al. agree- et good Ostro in by is images 1627 radar with of ment shape obtained The retrograde. > 2 – 1 Dcme,19)ad02 a Jnay 99;12 Ivar 1627 4 1999); (January, – mag 0.27 and 1998) (December, oie pc-ehd h eut r:63– 683 are: by results 1627) The and 15 (683 epoch-method. rota- asteroids an modified two of by a for senses calculated calculated and were been vec- tion periods have spin Sidereal resulting ellipsoids The amplitude-method. triaxial planets. and minor 3 tors for models new n h osblt farltvl atpeeso (P precession fast un- relatively a PG of possibility 1998 the suggest- Object ing lightcurve, Earth doubly-periodic showed Near ambiguously The 1999). (January, P edopitrqet to requests offprint Send 07(07.13.2) are: codes thesaurus later) Your hand by inserted be (will no. manuscript A&A . . . 2 2 0 λ 05 eateto xeietlPyis&Atooia Observa Astronomical & Physics Experimental of Department eateto hsclGorpy LEUiest,H-1088 University, ELTE Geography, Physical of Department us bevra okl Observatory Konkoly at Observer Guest / 3 =5 h p . olcigaldt rmteltrtr,w determined we literature, the from data all Collecting ± ± h 195 . 80 0, ± 30 = h . 0 0 3). . . ± ≥ 0 ;12 – 1627 2; 1, ± . .0mg 5 ldln 4 – Wladilena 852 mag; 0.40 5 P 05, 0 / 25 b/c h 1 . 210 , 1 .7mg(eebr 98 n .2mag 0.92 and 1998) (December, mag 0.77 01, 3 epeetnew present We ◦ y Szab´o Gy. , , oa ytm–mnrplanets minor – system solar 1 = sid ± β p 20 =0 λ . 09 52 = p ◦ d . , 145 = 1964156 ± β p [email protected] : 0 h . ± 30 = . 6 5 P 05, 1 ± / 15 , 3 325 0 n .S´arneczky K. and , R ± ◦ h ± . , sid ,01 a;75Aad – Amanda 725 mag; 0.13 2, 0 10 lee C observations CCD filtered ± a/b d . 000,rtord;852 retrograde; 0000001, =0 ◦ 8 , ◦ d . 1 = a/b , 1999154 h . β 62 p . 2 = 15 34 = ± 0 ± . h . 3 1 .2mag 0.32 01, ± ± ± 0 0 . 05, 0 d . 6 0000003, . ◦ 3, , 2 1 , b/c a/b =1 b/c 3 λ p h . = = = = 3, oy AEUiest,H62 zgd ´mte . Hungary D´om t´er 9., Szeged, H-6720 University, JATE tory, uaet uoiate . Hungary t´er 2., Ludovika Budapest, bevn u n osqetyw ol banol in- only obtain could the we consequently during and available run not per- observing were was filters task photometry other IRAF aperture Unfortunately the simple with a psf-photometry why formed of is use that the permit and an- not low did and resolution noises electronic gular high relatively The routines. summa- is 1. observations Table during of in background rized journal sky The the observations. with values compar- the by pixel at estimated peak be was the to parameter ing latter had the This ratio 10. than (SN) least signal-to-noise night) more to the night move secondly, from (varying to and profiles stellar allowed the not of FWHM were asteroids the etdsyae s2’1’wihcrepnst nangular an camera to 1 corresponds of CCD which pro- resolution 29’x18’ The is chip). AT200 area CCD sky coated jected Photometrics MCII 1600 a KAF data (1536x1024 The with Schmidt-telescope 1999. cm 60/90/180 January, ten equipped the to using on obtained 1998 were October, Observatory from Konkoly nights of Piszk´estet˝o Station ecridout carried We methods modelling and Observations 2. the with deals 3 Sect. while 2, results. minor observational Sect. 3 detailed in for discussed meth- are models to applied ods and and is limitations 1999 Oc- their paper Observations, January, between planets. this and out of 1998 carried aim and observations tober, CCD main (1999) new The al. present (1999). et S´arneczky al. in have project et Szab´o published this model of been to results order First already rotation. in and methods shape photometric their applica- different of enabling with tion asteroids lightcurves of multi-opposition consists available programme observing plan- minor The selected ets. of monitoring photometric to dressed solar recent or the into binarity evolution. insights system to yield may due they as lightcurves precession, multiperiodic e.g. effects, h mg euto a oewt tnadIRAF standard with done was reduction image The firstly, factors: two by limited were times exposure The esatdaln-emosrainlpoetad- project observational long-term a started We ′′ . 1/pixel. R C lee C bevtosat observations CCD filtered noao.digiphot.apphot.qphot ASTROPHYSICS ASTRONOMY AND . 2 Kiss et al.: CCD photometry and new models of 5 minor planets
Table 1. The journal of observations. (r – geocentric distance; ∆ – heliocentric distance; λ – ecliptic longitude; β – ecliptic latitude; α – solar phase angle; aspect data are referred to 2000.0)
Date RA Decl. r(AU) ∆(AU) λ β α 683 Lanzia 1998 12 14/15 00 12.78 +19 58.9 3.25 2.82 20 18 17 1998 12 16/17 00 13.78 +19 49.5 3.25 2.84 20 18 17 725 Amanda 1999 01 26/27 06 31.61 +27 13.5 2.34 1.44 110 24 12 852 Wladilena 1998 12 12/13 11 40.37 +27 28.2 2.98 2.71 163 23 19 1998 12 14/15 11 41.67 +27 31.9 2.98 2.68 163 23 19 1998 12 16/17 11 42.89 +27 36.2 2.98 2.65 163 23 19 1999 01 24/25 11 47.52 +30 52.9 2.95 2.18 170 19 14 1627 Ivar 1998 12 14/15 05 03.41 +10 30.4 2.22 1.26 76 −12 6 1998 12 15/16 05 02.00 +10 32.6 2.23 1.26 76 −12 6 1998 12 16/17 05 00.62 +10 34.9 2.23 1.27 76 −12 7 1999 01 22/23 04 30.95 +13 09.2 2.35 1.65 85 −13 20 1998 PG 1998 10 23/24 23 47.69 +09 15.0 1.23 0.26 2 9 25 1998 10 26/27 23 55.11 +08 26.9 1.23 0.27 2 7 25 1998 10 27/28 23 57.63 +08 11.6 1.23 0.27 2 7 26