WPC XIggB-%w\5 ~'C=+`JlL@cMqXmrpmI`汋 5q^ȑ:]ߌH11(QN)kژE}g%+1?!}Jf!ᕥp=B2-h5mSWWl& gcc(; z@3Sh~t{d4{av˜l([ȯFGZ?b Xo*|7? `۲uxs|6S 41 } |w&LZ!rxᒈO%)-cO/Q}z_[Iތ ôٛ?I9cxr2<;#;z"}0ĬYǒ&3b 7N.K\|[jaC1ox7Ɠ-U"v %U" 0IUN  CWfqas BI* BU @ D+9 0 0E AY^ H^ T 1````nX 0O #! N UL ^ N w@Z 4  m 1 1uN 0c ^ &^ 2^ >^ JfVaX^ l 1x<6X9`( CXH*0  C4 2Quick 1..0..(uH Z6Times New Roman Regular2dTable_A&0 d d d* `(CG TimesScalable'dxd Level 1 Level 2 Level 3 Level 4 Level 5(2u'$ 5w!   XX0XXXX0XXX0  ($ (    )   M << deUUn*ʣW*(UhCEKQW]cioAutoList31.1.1.1.1.1.1.1.3|w$ <6X9`( CXqx6X@QX@H*0  CXy*0 PQX(h5w$   XX0XXXX0XXX0HP LaserJet 6P/6MP - Enhanced0(uH Z4Times New Roman ItalicU* {  !"#$)U(5hCEKQW]cioAutoList11.1.1.1.1.1.1.1.##37=CIQYag1.a.i.(1)(a)(i)1)a)(;$25h  0  .3  0  ஖U*U*U*U*Table_ASU*(EhCEKQW]cioAutoList21.1.1.1.1.1.1.1. 5w!   XX0XXXX0XXX0  _X0XXX0  $'` $__NAME__________________________________      NEWTON'SLAWSANDTHEMASSESOFTHEPLANETS  b     0 '  1. ' SetupStarryNightbychoosinganequatorialorientationandturningoffthedaylight.Find  d Jupiter,thenchangethefieldofviewto3'.YoushouldseetheplanetJupiterandthemoonsasitwouldappearnowthroughatelescope. 0'(#'(# L Uh(##L0 '  2. ' 0''(#'(# $   0 '  $2Uh  2  .3  0''(#'(#  MeasurethediameterDofJupiterfrompoletopole,estimatingtothenearestmillimeter.Enter    thisvalueintotheDataTable.SincethediameterofJupiterisknowntobe143,000km,youcanestablishthescaleofthescreen.$݌ '(#'(# Ќ  0 ' Changethefieldofviewto15'.Sincethisaffectsthescale,ourcomputationforthescaleis: '(#'(#  '  ` ScaleforJupiter=143,000'5/XsZXXX0D ` #X0XXXsZ#Ԁ F 0 ' EnterthisscaleintheDataTable. '(#'(# 0 '  3. ' RightclickonJupitersmoonstoidentifyIo.ThenchooseShowOrbit.Measuretheorbital  diameterdofIo,againestimatingtothenearestmillimeter.EnterthisvalueintotheData  Table.Multiplybythescaletodeterminethetruediameteroftheorbitinkilometers,thenfinditsradiusabydividingthetruediameterby2.Whileaisinyourcalculator,computea3.Z'(#'(# 0 '  4. ' StartingataconvenientpointinIo'sorbit,likedirectlyinfrontorjustattheedgeoftheplanet, &v determinetherevolutionperiodpofIoindays,hoursandminutes.Youcanchangethehours  \ andminutesintheTimeTooltobringIotoyourstartinglocation,thendisplaytheJulianDateforthestartandrecorditintheTable.Againusingdays,hoursandminutes,letIocompleteonefullorbit.FindtheJulianDateforthefinishandrecorditintheTable.FromthedifferenceinthetwoJuliandates,computetheorbitalperiodpofIo.Thenfindp2andenteritintothe  Table. '(#'(# 0 '  5. ' Computetheratioa3/p2forIoandenterthisvalueintotheDataTable.V"!'(#'(# 0 '  6. ' IdentifytwootherGalileansatellitesEuropaandGanymede.Performthesamesteps3through "$r# 5todeterminethesizesaandtheorbitalperiodspofEuropaandGanymede.Enterallthese %X $ valuesintotheDataTable. '(#'(# L "5h((L $   $25h  7  .3  0 '   %X0XXX0ComputetheaveragevalueKJUPITERofa3/p2fromtheindividualKvaluesforIo,Europa,and#X0XX%X0 #&X0XXX0 ' #' Ganymede#X0XX&X0#%X0XXX0.#X0XX%X0#$݌(#('(#'(# Ќ   $   $25h  8  .3  0 '   ComputethemassofJupiterinkilograms.$݌l*%*'(#'(# Ќ   R+&+ * ddd Xdd Xdd X(#(#,` d4 ,D4 ,D4 ,D4 +  1 " b P1  XXXX0X0XX X  : 'J  :JUPITER V G/J"  P   PxVP@XX0  Po DiameterD,mmX0XP@ X0XX X  : '!h "  : M >&h  x P   PxMP@XX0  X0 Scale=143000*5/D : '! &"  : M >& &  x P   PxM ; ,! n "  ;IoX0XP@ X0XX X  ; ,! n "  ;P@XX0  X0 Europa ? ,! n "  ?Ganymede XX # X X# S D, n " x P   qxSOrbitd,mm ; ,!f "  ; 2 #f   2 - f   - J ;#f  x q   qxJd'Scale ; ,! "  ; 2 #   2 -    - J ;#  x q   qxJRadiusa ; ,!F "  ; 2 #F   2 - F   - J ;#F  x q   qxJa3 ; ,!> "  ; 2 #>   2 - >   - E 6#>  x q   xEJDstart 2 #! "  2 )    ) -    - @ 1 ! x   x@JDfinish 2 #!""  2 ) #  ) - $  - E 6% x   qxEPeriodp=JDfJDs ; ,!f&"  ; 2 #f'  2 - f(  - J ;#f) x q   qxJp2 ; ,!^*"  ; 2 #^+  2 - ^,  - J ;#^- x q   qxJK=a3/p2 ; ,!."  ; 2 #/  2 - 0  - E 6#1 x q   xE C 0!>2"  C >3 ThesethreeKvaluesshouldbeapproximatelyequaltoeachother.Ifnot,gobacktodeterminethereason.Ifso,computetheiraveragebelow. Q B*n5" x   qxQAverageKJUPITER : '!6"  : O >&7 x q   x@OMassm : '!N8"  :'TT '9'Ӏm=!2'4'KJUPITER/G= kg # 2 P@# 6,*N9 x@     6<(#G=4.98'1010 : 0    (#(# _  !n= '',TTP' XX  2'',TTP'*'` ,'**` ,'* $   X0XX X$$25h  9  .3  0 '   NowletusgoafterSaturn.Findtheplanet,changethefieldofviewto1',andmeasurethe  diameterDofSaturnfrompoletopole,estimatingtothenearestmillimeter.Enterthisvalue f intotheDataTable.SincethediameterofSaturnisknowntobe121,000km,youcanestablishthescaleofthescreen.$$$݌ '(#'(# Ќ  0 ' Changethefieldofviewto7'.Sincethisaffectsthescale,ourcomputationforthescaleis: '(#'(#  '  ` Scalefor##$$#Saturn##Jupiter#=121,000*7/# XXXX0$#XsZXX XD    # XXXXsZ'#Ԁ   0 ' EnterthisscaleintheDataTable. '(#'(#  $   $(25h  10  .3  0 '   RightclickonSaturnsmoonstoidentifyTitan.ThenchooseShowOrbit.Measurethe   orbitaldiameterdofTitan,againestimatingtothenearestmillimeter.Enterthisvalueinto p  theDataTable.Multiplybythescaletodeterminethetruediameteroftheorbitinkilometers,thenfinditsradiusabydividingthetruediameterby2.Whileaisinyour P calculator,computea3.$((݌@'(#'(# Ќ  0 '  11. ' StartingataconvenientpointinTitan'sorbit,determinetherevolutionperiodpofTitanin  p days,hoursandminutes.YoucanusetheedgeoftheTimeToolforyourstartfinishline.YoucanchangethehoursandminutesintheTimeTooltobringTitantoyourstartinglocation,thendisplaytheJulianDateforthestartandrecorditintheTable.Againusingdays,hoursandminutes,letTitancompleteonefullorbit.FindtheJulianDateforthefinishandrecorditintheTable.FromthedifferenceinthetwoJuliandates,computetheorbitalperiodpofTitan.Thenfindp2andenteritintotheTable.'(#'(# 0 '  12. ' Computetheratioa3/p2forTitanandenterthisvalueintotheDataTable.'(#'(# 0 '  13. ' IdentifytwoothersatellitesRheaand_Dione_.Performthesamesteps10through12to   determinethesizesaandtheorbitalperiodspofRheaand_Dione_.Enterallthesevaluesinto p! theDataTable. '(#'(#   L ,Eh(("L $   $02Eh  14  .3  0 '   Computetheaveragevalue_KSATURN_ofa3/p2fromtheindividualKvaluesforTitan,Rhea, @$" and_Dione_'X0XX X.# XXX'X02#X0XX X$00݌0% #'(#'(# Ќ   $   $22Eh  15  .3  0 '   ComputethemassofSaturninkilograms.$22݌'V"%'(#'(# Ќ  + ''` 5$+  '<#& _*)* dd` d4 ` D4 D4 D4 (#(#,` d4 ,D4 ,D4 ,D4 +  1 " b P1P@XX0# 2 P@E2#P@  2 : 'J  :"#X0XP@)5#"SATURN"P@XX0" V G/J"  P   PxV# XXXX0B2#DiameterD,mm+X0XX X : '!h "  : M >&h  x P   PxM# XXX+X05#Scale=121000*7/D : '! "  : M >&   x P   PxM ; ,! H "  ;Titan+X0XX X ; ,! H "  ;# XXX+X07#Rhea+X0XX X ? ,! H "  ?# XXX+X08#_Dione_ S D, H " x P   qxSOrbitd,mm ; ,!@ "  ; 2 #@   2 - @   - J ;#@  x q   qxJd'Scale ; ,! "  ; 2 #   2 -    - J ;#  x q   qxJRadiusa ; ,! "  ; 2 #   2 -    - J ;#  x q   qxJa3 ; ,!h "  ; 2 #h   2 - h   - E 6#h  x q   xEJDstart 2 #!` "  2 ) `   ) - `   - @ 1` ! x   x@JDfinish 2 #!""  2 ) #  ) - $  - E 6% x   qxEPeriodp=_JDf_Ԁ_JDs_ ; ,!@&"  ; 2 #@'  2 - @(  - J ;#@) x q   qxJp2 ; ,!8*"  ; 2 #8+  2 - 8,  - J ;#8- x q   qxJK=a3/p2 ; ,!."  ; 2 #/  2 - 0  - E 6#1 x q   xE C 0!2"  C 3 ThesethreeKvaluesshouldbeapproximatelyequaltoeachother.Ifnot,gobacktodeterminethereason.Ifso,computetheiraveragebelow. Q B*H5" x   qxQAverage_KSATURN_ : '!6"  : O >&7 x q   x@OMassm : '!(8"  :'TT ''Ӏm=!2'4'_KSATURN_/G= kg6,*(9 x@     622<(#G=4.98'1010# 2 P@u5## XX  2+6# : 0   0(#(# (#(# !'',TTP'!16.0 '   ThemassoftheEarthis6.0'1024kg.ComputethemassesofJupiterandSaturninunits ("x> oftheEarthsmass(MQ).G#h?'(#'(#   $ '` '$0 ' 0` '(#'(#MassofJupiter=____________MQ$H A` (#` (# 0 ' 0` '(#'(#MassofSaturn=____________MQ&("C` (#` (# X0XX XUXX0>(#14March2001#X0XUI## XXXX0H#