\PERGAMON Planetary and Space Science 36 "0888# 252Ð272
9921Ð9522:88:, ! see front matter Þ 0888 Elsevier Science Ltd[ All rights reserved[PII] S 9 9 2 1 Ð 9 5 2 2 " 8 7 # 9 9 0 0 4 Ð 8
Three years of Ulysses dust data] 0882Ð0884H[ Kru�gera\�\ E[ Gru�na\ M[ Landgrafa\ M[ Baguhla\ S[ Dermottb\ H[ Fechtiga\
B[A[ Gustafsonb\ D[P[ Hamiltonc\ M[S[ Hannerd\ M[ Hora�nyie\ J[ Kissela\B[A[ Lindbladf\ D[ Linkerta\ G[ Linkerta\ I[ Manng\ J[A[M[ McDonnellh\ G[E[ Mor_lli\
C[ Polanskeyd\ G[ Schwehmj\ R[ Sramaa\ H[A[ Zookk
a Max!Planck!Institut fu�r Kernphysik\ 58918 Heidelber`\ Germanyb University of Florida\ Gainesville\ FL 21500\ U[S[A[
c University of Maryland\ Colle`e Park\ MD 19631!1310\ U[S[A[d Jet Propulsion Laboratory\ Pasadena\ CA 80098\ U[S[A[
e Laboratory for Atmospheric and Space Physics\ University of Colorado\ Boulder\ CO 79298\ U[S[A[f Lund Observatory\ 110 Lund\ Sweden
g Max!Planck!Institut fu�r Aeronomie\ 26080 Katlenbur`!Lindau\ Germanyh University of Kent\ Canterbury CT1 6NR\ U[K[
i Max!Planck!Institut fu�r Extraterrestrische Physik\ 74637 Garchin`\ Germanyj ESTEC\ 1199 AG Noordwijk\ The Netherlands
k NASA Johnson Space Center\ Houston\ TX 66947\ U[S[A[
Received 8 April 0887^ received in revised form 17 September 0887^ accepted 1 October 0887
Abstract
The Ulysses spacecraft is orbiting the Sun on a highly inclined ellipse "i � 68>#[ After its Jupiter ~yby in 0881 at a heliocentricdistance of 4[3 AU\ the spacecraft reapproached the inner solar system\ ~ew over the Sun|s south polar region in September 0883\crossed the ecliptic plane at a distance of 0[2 AU in March 0884\ and ~ew over the Sun|s north polar region in July 0884[ We reporton dust impact data obtained with the dust detector onboard Ulysses between January 0882 and December 0884[ We publish andanalyse the complete data set of 498 recorded impacts of dust particles with masses between 09−05 gÐ09−6 g[ Together with 857 dustimpacts from launch until the end of 0881 published earlier "Gru�n et al[\ 0884c#\ information about 0366 particles detected with theUlysses sensor between October 0889 and December 0884 is now available[ The impact rate measured between 0882 and 0884 stayedrelatively constant at about 9[3 impacts per day and varied by less than a factor of ten[ Most of the impacts recorded outside about2[4 AU are compatible with particles of interstellar origin[ Two populations of interplanetary particles have been recognized] bigmicrometer!sized particles close to the ecliptic plane and small sub!micrometer!sized particles at high ecliptic latitudes[ The observedimpact rate is compared with a model for the ~ux of interstellar dust particles which gives relatively good agreement with theobserved impact rate[ No change in the instrument|s noise characteristics or degradation of the channeltron could be revealed duringthe three!year period[ Þ 0888 Elsevier Science Ltd[ All rights reserved[
0[ Introduction
The Ulysses mission is exploring the solar systembetween 0 and 4[3 AU from the Sun over a wide range ofecliptic latitudes "−68>Ц68>#[ Ulysses carries a multi!coincidence impact ionization detector\ which is nearlyidentical to the dust detector ~own onboard the Galileospacecraft[ Detailed descriptions of the dust instrumentsonboard both spacecraft have been published by Gru�n etal[ "0881a\ b^ 0884a#[ Early results on interplanetary dustobtained from both missions and dust measurements
� Corresponding author[ Fax] ¦38 5110 405 213^ e!mail] kruegerÝgalileo[mpi!hd[mpg[de
achieved by Ulysses in the environment of Jupiter havebeen reported "Gru�n et al[\ 0881c\ d^ Gru�n\ 0883#[ Unex!pected intermittent streams of dust particles originatingfrom the Jovian system and interstellar particles sweepingthrough the solar system were discovered by Ulysses"Gru�n et al[\ 0882#[ A detailed analysis of the completeUlysses dust data has led to the identi_cation of {small|impacts that had been previously considered potentialnoise events "Baguhl et al[\ 0882#[
Data from the dust instruments onboard both space!craft*Ulysses and Galileo*have been used in variousways] asteroids and comets have been investigated as dustsources "Riemann and Gru�n\ 0881^ Hamilton and Burns\0881^ Gru�n et al[\ 0883a^ Mann et al[\ 0885a#^ conse!
H[ Kru�`er et al[ : Planetary and Space Science 36 "0888# 252Ð272253
quences for the zodiacal light and other interplanetarymeteoroid measurements have been considered "Mann etal[\ 0881^ Mann and Gru�n\ 0882^ Mann et al[\ 0885b^Taylor et al[\ 0885#^ a detailed model of interplanetarymeteoroid populations in the solar system has beendeveloped "Divine\ 0882^ Divine et al[\ 0882^ Gru�n andStaubach\ 0885^ Gru�n et al[\ 0886#^ the dust streams orig!inating from the Jovian system have been analysed "Hor!a�nyi et al[\ 0882a\ b^ Hamilton and Burns\ 0882^ Zook etal[\ 0885# and\ _nally\ the properties of interstellar dustin the heliosphere have been investigated "Gru�n et al[\0883b^ Baguhl et al[\ 0884a\ b^ 0885^ Landgraf and Gru�n\0887#[
This is the _fth paper in a series dedicated to presentingboth raw and reduced data obtained from the dust instru!ments onboard the Ulysses and Galileo spacecraft[ Gru�net al[ "0884a^ hereafter\ Paper I# describe the reductionprocess of Ulysses and Galileo dust data[ Papers II andIII "Gru�n et al[\ 0884b\ c# present the data sets from theinitial three and two years of the Galileo and Ulyssesmissions\ respectively[ In the case of Ulysses the timeperiod covered "Paper III# was October 0889ÐDecember0881[ In the current paper we extend the Ulysses data setfrom January 0882 until December 0884[ In a companionpaper "Kru�ger et al[\ 0887\ Paper IV#\ we publish theGalileo data set for the same time period[ The main dataproducts are a table of the impact rate of all impactsdetermined from the particle accumulators and a table ofboth raw and reduced data of all dust impacts transmittedto Earth[ The information presented in these papers issimilar to data which we are submitting to the variousdata archiving centers "Planetary Data System\ NSSDC\Ulysses Data Center\ etc[#[ Electronic access to the datais also possible via the world wide web] http]::galileo[mpi!hd[mpg[de[
This paper is organised similarly to Paper III[ Section1 gives a brief overview of the Ulysses mission and listsimportant mission events from 0882Ð84[ A description ofthe Ulysses dust data set for this period is given in Section2[ Sections 3 and 4 analyse and discuss the new data set[
1[ Mission and instrument operation
Ulysses was launched on 5 October 0889 and wasbrought onto a direct trajectory towards Jupiter[ Aswing!by maneuvre at Jupiter on 7 February 0881de~ected the spacecraft into an orbit that is inclined by68> to the ecliptic plane "Fig[ 0#[ In October 0883 Ulyssespassed the Sun|s south polar region\ then crossed theecliptic plane again\ this time at a perihelion distance of0[2 AU on 01 March 0884 and ~ew over the Sun|s northpolar region in August 0884[ In April 0887 the spacecraftcrossed the ecliptic plane at its aphelion at 4[3 AU[Approximate orbital elements for the Ulysses trajectorythat include the whole out!of!ecliptic part of its orbit\ aregiven in Paper III[
Fig[ 0[ Three!dimensional view of Ulysses| interplanetary trajectoryfrom launch until the end of 0885 in ecliptic coordinates[ The Sun is inthe center[ The orbits of Earth and Jupiter indicate the ecliptic plane[The initial trajectory of Ulysses was in the ecliptic plane[ During Jupiter~yby in early 0881 Ulysses was brought into an orbit with 68> inclinationthat sent the spacecraft close to the ecliptic poles[ Crosses mark thespacecraft position at the beginning of each year[ Vernal equinox is tothe right "positive x axis#[
Ulysses is a spin!stabilized spacecraft with its spin axispointing towards Earth[ In Fig[ 1 we show the deviationof the spin axis from the nominal Earth direction for theperiod 0882 to 0884 considered in this paper[ Most of thetime the axis pointing was within one degree of the Earthdirection[ This rather small deviation is negligible for theconsiderations in this paper[ The Ulysses spacecraft andmission are explained in more detail by Wenzel et al["0881#[ Details about the data transmission to Earth canalso be found in Paper III[
The dust detector onboard Ulysses "GRU# has a 039>wide _eld of view[ The instrument is mounted nearlyat right angles "74># to the antenna pointing direction"spacecraft spin axis#[ Therefore\ the sensor is most sen!sitive to particles approaching from the plane per!pendicular to the spacecraftÐEarth direction[ The
Fig[ 1[ Spacecraft attitude] deviation of the antenna pointing direction"i[e[\ negative spin axis# from the nominal Earth direction[ The anglesare given in ecliptic longitude "top# and latitude "bottom\ equinox0849[9#[
H[ Kru�`er et al[ : Planetary and Space Science 36 "0888# 252Ð272 254
rotation angle measures the sensor viewing direction atthe time of a dust impact[ During one spin revolution therotation angle scans through a complete circle of 259>[The 9> rotation angle is de_ned to be the direction closestto ecliptic north[ At high ecliptic latitudes\ however\ thesensor pointing at 9> rotation angle signi_cantly deviatesfrom the actual north direction[ During the passages overthe Sun|s polar regions the sensor always scans througha plane tilted by about 29> from the ecliptic and allrotation angles lie close to the ecliptic plane "cf[ Fig[ 3 inGru�n et al[\ 0886#[ A sketch of the viewing geometry canbe found in Gru�n et al[ "0882#[
Table 0 lists signi_cant mission and dust instrumentevents from 0882Ð84[ Earlier events are only listed ifespecially signi_cant[ A comprehensive list of events fromlaunch until the end of 0881 is given in Paper III[ Duringthe early phases of the mission the in!orbit noise charac!teristics of the instrument were investigated "Paper III#[This led to a relatively noise!free con_guration "hereaftercalled nominal con_guration# for the instrument after 09February 0881] channeltron voltage 0039 V "HV�2#^event de_nition status such that either the channeltronor the ion!collector channel can\ independent of eachother\ start a measurement cycle "EVD�C\ I#^ detectionthresholds for ion!collector\ channeltron and electron!channel set to the lowest levels and the detection thr!eshold for the entrance grid set to the _rst digital step"SSEN�9\ 9\ 9\ 0#[ See Paper I for a description of theseterms[
The operational con_guration of the dust instrumentwas changed several times during noise tests] startingfrom the nominal con_guration described above\ all testshave been performed with the same instrument settings[During noise tests\ the following changes of the instru!ment con_guration were applied at one!hour intervals]"a# set the event de_nition status such that the chan!neltron\ the ion collector and the electron!channel caninitiate a measurement cycle "EVD�C\ I\ E#^ "b# set thethresholds for all channels to their lowest levels"SSEN�9\ 9\ 9\ 9#^ "c# reset the event de_nition statusto its nominal con_guration "EVD�C\ I#^ "d# increasethe channeltron high voltage by one digital step"HV�3#^ "e# reset the channeltron high voltage and thedetection thresholds to their nominal settings "HV�2\SSEN�9\ 9\ 9\ 0#[ After step "e# the instrument is backin its nominal con_guration[ No detectable change in thenoise behavior was revealed by the noise tests during thethree years from 0882Ð84[
Spacecraft anomalies occurred _ve times between 0882and 0884\ and all scienti_c instruments onboard wereswitched o} automatically for about one day during so!called DNELs "Disconnect all Non!Essential Loads#[After each DNEL\ the dust instrument was switched onagain and was con_gured to its nominal operationalmode[
The dust instrument has two heaters to allow for a
relatively stable operating temperature within the sensor[By heating one of the two or both heaters\ three di}erentheating power levels can be achieved "399\ 799 or 0199mW#[ One or both heaters were switched on most of thetime\ except close to the Sun between 4 February and 01June 0884 when both were switched o}[ The heatersremained switched on during the DNELs[ Table 0 liststhe total heating powers provided by the heaters[ Thetemperature of the dust sensor was between −19>CЦ04>C[
A timing error in the instrument electronics led towrong spacecraft sector information for about 19) ofthe events in the data set published earlier "cf[ PaperIII\ indicated by ROT�888 in Table 3#[ The error wascorrected by a reprogramming of the instrument on 29April 0882[
After launch of Ulysses the sounder of the URAPinstrument "Stone et al[\ 0881# emerged as a signi_cantand unexpected noise source for the dust sensor[ Whenthe sounder was switched on after launch\ sounder inter!ference caused about 19) dead time "Paper III#[ Withthe sounder now usually being operated at a lower rateof about 1 min at 1 h intervals the dead time is reducedto about 1)[ In a detailed investigation of the noisebehavior of the Ulysses dust instrument Baguhl et al["0882# showed that the noise rate measured during per!iods of sounder operation was correlated with the dis!tance to\ and the position of\ the Sun with respect to thesensor!viewing direction] most noise events are triggeredwhen the Sun shines directly into the sensor[ On theother hand\ when the spacecraft was at large heliocentricdistances in 0882\ the noise rate was extremely low\ evenduring sounder operation periods[
In Fig[ 2 we show the noise rate for the 0882Ð84 period[The upper panel shows the daily maxima\ which aredominated by interference with the sounder[ Since thesounder was operated for periods of only 1 min with quietintervals of about 1 h\ such high noise rates prevailed onlyduring about 1) of the time\ with the remaining 87)being free of sounder noise[ In 0883 the maxima in thenoise rate induced by the sounder began to increase sig!ni_cantly when Ulysses approached the inner solarsystem[ The highest sounder noise rates occurred aroundperihelion passage in March 0884[ From 01Ð11 July 0883and 13 NovemberÐ0 December 0883\ the sounder wasswitched o} and the noise level dropped to about 09events per day[ The noise during quiet times when thesounder was switched o} is shown in the lower panel ofFig[ 2[ The average was about 19 events per day whichshows that the dust instrument was not a}ected by deadtime caused by random noise events during 87) of thetime[
2[ Impact events
Impact events are classi_ed into four classes and sixion charge amplitude ranges which lead to 13 individual
H[ Kru�`er et al[ : Planetary and Space Science 36 "0888# 252Ð272255
Table 0Ulysses mission and dust detector "GRU# con_guration\ tests and other events[ Only selected events before 0882 aregiven[ See Section 1 for details
YearÐday Date Time Event
89Ð168 95[09[89 Ulysses launch80Ð043 92[95[80 07]02 GRU heater on] 0199 mW81Ð930 09[91[81 06]99 GRU nominal con_guration] HV � 2\ EVD � C\ I\ SSEN � 999082Ð934 03[91[82 95]42 Ulysses DNEL è182Ð934 03[91[82 11]49 GRU on\ nominal con_guration82Ð019 29[93[82 91]35 GRU new program "FN6 data# load82Ð015 95[94[82 12]96 GRU start new program82Ð085 04[96[82 91]99 GRU noise test82Ð195 14[96[82 90]99 GRU HV � 382Ð100 29[96[82 95]92 GRU HV � 282Ð110 98[97[82 01]06 Ulysses DNEL è282Ð112 00[97[82 11]25 GRU on82Ð113 01[97[82 96]32 GRU nominal con_guration82Ð120 08[97[82 90]48 GRU noise test82Ð148 05[98[82 00]48 GRU noise test82Ð176 03[09[82 07]48 GRU noise test82Ð204 00[00[82 08]48 GRU noise test82Ð220 16[00[82 12]30 Ulysses DNEL è382Ð221 17[00[82 04]10 GRU on82Ð221 17[00[82 11]47 GRU nominal con_guration82Ð232 98[01[82 07]99 GRU noise test83Ð995 95[90[83 05]99 GRU noise test83Ð923 92[91[83 03]48 GRU noise test83Ð951 92[92[83 96]99 GRU noise test83Ð989 20[92[83 97]34 GRU noise test83Ð007 17[93[83 96]29 GRU noise test83Ð035 15[94[83 94]99 GRU noise test83Ð063 11[95[83 95]99 GRU noise test83Ð191 10[96[83 92]48 GRU noise test83Ð129 07[97[83 91]48 GRU noise test83Ð147 04[98[83 99]99 GRU noise test83Ð165 92[09[83 Ulysses South polar pass "lat[ −68>\ 1[0 AU#83Ð170 97[09[83 99]29 GRU heater] 799 mW83Ð172 09[09[83 07]34 Ulysses DNEL è483Ð173 00[09[83 12]95 GRU on83Ð174 01[09[83 93]06 GRU nominal con_guration83Ð175 02[09[83 08]48 GRU noise test83Ð203 09[00[83 93]48 GRU noise test83Ð230 97[01[83 12]48 GRU noise test83Ð994 94[90[84 99]99 GRU noise test84Ð992 91[91[84 90]48 GRU noise test84Ð925 94[91[84 90]13 GRU heater o}84Ð960 01[92[84 01]90 Ulysses ecliptic plane crossing and perihelion "0[2 AU#84Ð041 90[95[84 92]48 GRU noise test84Ð052 01[95[84 92]20 GRU heater on] 399 mW84Ð079 18[95[84 92]48 GRU noise test84Ð197 16[96[84 93]99 GRU noise test84Ð105 93[97[84 99]40 GRU heater] 799 mW84Ð120 08[97[84 Ulysses North polar pass "lat[ ¦68>\ 1[0 AU#84Ð125 13[97[84 04]48 GRU noise test84Ð153 10[98[84 07]48 GRU noise test84Ð181 08[09[84 08]48 GRU noise test84Ð299 16[09[84 05]12 GRU heater] 0199 mW84Ð219 05[00[87 98]48 GRU noise test84Ð233 09[01[84 04]44 Ulysses DNEL è584Ð233 09[01[84 10]17 GRU on84Ð235 01[01[84 97]43 GRU nominal con_guration84Ð237 03[01[84 04]99 GRU noise test
Abbreviations used] DNEL] Disconnect non!essential loads "i[e[\ all scienti_c instruments#^ HV] channeltron highvoltage step^ EVD] event de_nition\ ion! "I#\ channeltron! "C#\ or electron!channel "E#^ SSEN] detection thresholds\ICP\ CCP\ ECP and PCP[
H[ Kru�`er et al[ : Planetary and Space Science 36 "0888# 252Ð272 256
Fig[ 2[ Noise rate "class 9 events# detected with the dust instrument[Upper panel] Daily maxima in the noise rate "determined from theAC90 accumulator#[ The sounder was operated for only 1) of the totaltime\ and the daily maxima are dominated by sounder noise[ Sharpspikes are caused by periodic noise tests and short periods of recon!_guration after DNELs "cf[ Table 0#[ From 01Ð11 Jul[ 0883 and 13Nov[ to 0 Dec[ 0883 the sounder was not operated\ which reduced themaximum noise by several orders of magnitude[ Lower panel] Noiserate detected during quiet intervals when the sounder was switched o}\which was the case about 87) of the time "one!day average calculatedfrom the number of AC90 events for which the complete informationhas been transmitted to Earth#[
categories[ In addition\ the instrument has 13 accumu!lators with one accumulator belonging to one individualcategory[ Class 2\ our highest class\ are real dust impactsand class 9 are noise events[ Depending upon the noiseof the charge measurements\ classes 0 and 1 can be truedust impacts or noise events[ This classi_cation schemefor impact events has been described in Paper I and thisscheme is still valid for the Ulysses dust instrument[ Incontrast to the Galileo dust instrument which had tobe reprogrammed because of the low data transmissioncapabilities of the Galileo spacecraft\ no such repro!gramming was necessary for Ulysses[ Most of the dataprocessing for Ulysses is done on the ground[
Between 0 January 0882 and 20 December 0884 thecomplete data "sensor orientation\ charge amplitudes\charge rise times\ etc[# of 61\798 events including 498dust impacts were transmitted to Earth[ Table 1 lists thenumber of all dust impacts counted with the 13 accumu!lators of the dust instrument[ {ACxy| refers to class num!ber {x| and amplitude range {y| "for a detailed descriptionof the accumulator categories see Paper I#[ As discussed
in the previous section\ most noise events were recordedduring the short time periods when either the sounder ofthe URAP instrument was operating "cf[ Paper III# orthe dust instrument was con_gured to its high sensitivestate for noise tests\ or both[ During these periods manyevents were only counted by one of the 13 accumulatorsbecause their full information was overwritten before thedata could be transmitted to Earth "see bottom of Table1#[ Since the dust impact rate was low during times sur!rounding these periods\ it is expected that only a few truedust impacts were lost[
Two particles in AC21 and AC22 "days 82Ð043\ 10]90h and 82Ð208\ 04]20 h#\ respectively\ were detected in agap of several hours when no data could be transmittedto Earth\ and their full information had to be taken fromthe instrument memory "FN6\ cf[ Gru�n et al[\ 0881a#[Before and after these gaps the sounder was operated forabout 1 min at 1 h intervals and we assume that it wasoperated with the same frequency in the gap[ Due tothese long quiet intervals between sounder operation it israther unlikely that the two events occurred when thesounder was active[ Even in such a case these are stillvery likely true dust impacts because the sounder noiseusually a}ects only the lowest ion amplitude range"AR0#[
All 498 dust impacts detected between 0882 and 0884for which the complete information exists are listed inTable 2[ Dust particles are identi_ed by their sequencenumber and their impact time "_rst two columns#[ Theevent category*class "CLN# and amplitude range"AR#*are given in the third and fourth columns[ Rawdata as transmitted to Earth are shown in the next col!umns] sector value "SEC# which is the spacecraft spinorientation at the time of impact\ impact charge numbers"IA\ EA\ CA# and rise times "IT\ ET#\ time di}erenceand coincidence of electron and ion signals "EIT\ EIC#\coincidence of ion and channeltron signal "IIC#\ chargereading at the entrance grid "PA# and time "PET# betweenthis signal and the impact[ Then the instrument con!_guration is given] event de_nition "EVD#\ charge sensingthresholds "ICP\ ECP\ CCP\ PCP# and channeltron highvoltage step "HV#[ Compare Paper I for further expla!nation of the instrument parameters[
The next four columns in Table 2 give informationabout Ulysses| orbit] heliocentric distance "R#\ eclipticlongitude and latitude "LON\ LAT# and distance fromJupiter "DJup#[ The next column gives the rotation angle"ROT# as described in Section 1[ Whenever this value isunknown\ ROT is arbitrarily set to 888[ This occurs 03times[ Then follows the pointing direction of the dustinstrument at the time of particle impact in ecliptic longi!tude and latitude "SLON\ SLAT#[ When ROT is not validSLON and SLAT are useless and are also set to 888[ Meanimpact velocity "V# and velocity error factor "VEF\ i[e[\multiply or divide stated velocity by VEF to obtain upperor lower limits# as well as mean particle mass "M# and
H[ Kru�`er et al[ : Planetary and Space Science 36 "0888# 252Ð272257
Table 1Overview of dust impacts accumulated with the Ulysses dust detector between 0 January 0882 and 20 December 0884[ Switch!on of the instrumentis indicated by horizontal lines[ The heliocentric distance R\ the lengths of the time interval Dt "days# from the previous table entry\ and thecorresponding numbers of impacts are given for the 13 accumulators[ The accumulators are arranged with increasing signal amplitude ranges "AR#\with four event classes for each amplitude range "CLN � 9\ 0\ 1\ 2#^ e[g[\ AC20 means counter for AR � 0 and CLN � 2[ The Dt in the _rst line "82Ð990# is the time interval counted from the last entry in Table 2 in Paper III[ The totals of counted impacts�\ of impacts with complete data\ and ofall events "noise plus impact events# for the entire period are also given
Date Time R Dt AC AC AC AC AC AC AC AC AC AC AC AC AC AC AC AC AC AC AC AC AC AC AC AC"h# "AU# "d# 90� 00� 10 20 91� 01 11 21 92 02 12 22 93 03 13 23 94 04 14 24 95 05 15 25
82Ð990 91]97 4[954 1[0 * * * * * * * * * * * * * * * * * * * * * * * *82Ð997 98]13 4[938 6[2 * 0 * * * * * 1 * * * 1 * * * * * * * * * * * *82Ð905 91]40 4[917 6[6 0 * * * 0 * * 1 * * * * * * * * * * * * * * * *82Ð912 92]99 4[900 6[9 0 * * * * 0 * * * * * * * * * * * * * * * * * *82Ð929 96]04 4[990 6[1 * * * * * * * 0 * * * 0 * * * * * * * * * * * *
82Ð933 07]49 3[856 03[4 0 0 * 0 * 0 * 0 * * * * * * * * * * * * * * * *82Ð934 03]42 3[841 9[782Ð942 91]02 3[820 6[4 * * * * 0 * * 1 * 0 * 1 * * * * * * * * * * * *82Ð959 95]96 3[818 6[1 * * * * * * * * * * * * * * * * * * * * * * * *82Ð957 94]18 3[777 7[9 1 * * * * * * * * * * * * * * * * * * * * * * *
82Ð965 90]37 3[778 6[7 0 * * * 0 * * 1 * * * 0 * * * * * * * * * * * *82Ð972 92]37 3[769 6[0 0 * * * * * * 1 * * * 0 * * * * * * * * * * * *82Ð989 93]93 3[741 6[9 * 0 * * 0 * * 2 * * * 0 * * * * * * * * * * * *82Ð987 91]14 3[685 6[8 0 * * * * 1 * 0 * * * * * * * * * * * * * * * *82Ð094 93]49 3[709 6[0 0 0 * * * 0 * * * * * * * * * * * * * * * * * *
82Ð002 99]97 3[677 6[7 * 0 * * * * * 0 * * * * * * * * * * * * * * * *82Ð019 99]26 3[657 6[9 0 * * * * * * 1 * * * * * * * 0 * * * * * * * *82Ð016 90]09 3[636 6[9 0 * * * * * 0 * * * * * * * * * * * * * * * * *82Ð023 93]37 3[615 6[1 * * * 0 * * * * * * * * * * * * * * * * * * * *82Ð031 99]21 3[691 6[7 * * * * * * * * * * * * * * * * * * * * * * * *
82Ð038 90]14 3[579 6[9 * * * * * 0 * * * * * * * * * * * * * * * * * *82Ð045 91]26 3[486 6[0 0 * * * * * * * * * * 0 * * * * * * * * * * * *82Ð053 90]44 3[522 7[9 1 * * * * * * * * * 0 * * * * * * * * * * * *82Ð060 91]31 3[439 6[9 * * * * * * * * * * * * * * * * * * * * * * * *82Ð068 90]22 3[472 7[9 * * * * * * * 0 * * * 0 * * * * * * * * * * * *
82Ð076 00]18 3[365 7[3 * * * * * * * * * * * * * * * * * * * * * * * *82Ð084 90]95 3[418 6[5 * * * * * * * 0 * * * * * * * * * * * * * * * *82Ð191 90]38 3[494 6[9 * * * * * 0 * * * * * * * * * * * * * * * * * *82Ð109 99]98 3[365 6[8 * * * * * * * * * * * 0 * * * * * * * * * * * *82Ð106 99]00 3[340 6[9 * * * * * 0 * * * * * 0 * * * * * * * * * * * *
82Ð113 95]03 3[313 6[2 0 * * * * * * * * * * 0 * * * * * * * * * * * *82Ð114 95]18 3[310 0[982Ð122 90]12 3[281 6[7 0 * * * * * * 0 * * * * * * * * * * * * * * * *82Ð130 92]44 3[250 7[0 0 * * * * * 0 0 * * * 1 * * * * * * * * * * * *82Ð138 91]30 3[109 6[8 0 * * 0 * * * * * * * * * * * * * * * * * * * *
82Ð146 90]12 3[188 6[8 * * * * 0 * * * * * * * * * * * * * * * * * * *82Ð154 09]19 3[155 7[3 * * * * * 0 * 0 * * * * * * * * * * * * * * * *82Ð162 90]93 3[124 6[5 1 * * * * * * 1 * * * * * * * * * * * * * * * *82Ð170 90]04 3[191 7[9 * * * * * 0 0 * * * * 0 * * * * * * * * * * * *82Ð177 91]44 3[910 6[0 0 * * * 0 * * * * * * * * * * * * * * * * * * *
82Ð185 95]00 3[027 7[0 * 0 * * * 0 * * * * * * * * * * * * * 0 * * * *82Ð293 99]32 3[094 6[7 * * * * * * * 0 * * * 1 * * * 0 * * * * * * * *82Ð201 91]32 2[787 7[0 0 * * * * * * * * * * 0 * * * * * * * * * * * *82Ð219 92]38 3[923 7[9 1 * * * * * * 1 * * * * * * * * * * * * * * * *82Ð220 06]10 2[681 00[5 3 * * * * 0 * 0 * * * 0 * 0 * * * * * * * * * *
continued
H[ Kru�`er et al[ : Planetary and Space Science 36 "0888# 252Ð272 258
Table 1*continued
Date Time R Dt AC AC AC AC AC AC AC AC AC AC AC AC AC AC AC AC AC AC AC AC AC AC AC AC"h# "AU# "d# 90� 00� 10 20 91� 01 11 21 92 02 12 22 93 03 13 23 94 04 14 24 95 05 15 25
82Ð221 06]11 2[675 0[982Ð239 90]18 2[832 6[2 * * * * * * * * * * * * * * * * * * * * * * * *82Ð237 99]35 2[895 7[9 0 * * * 0 * * * * * * 1 * * * 0 * * * * * * * *82Ð245 99]05 2[757 7[9 * * * * * * * * * * * 0 * * * * * * * * * * * *82Ð252 99]38 2[723 6[9 * * * * * * * * * * * * * * * * * * * * * * * *
83Ð995 90]91 2[684 7[9 0 0 * * * * * * * * * 1 * * * * * * * * * * * *83Ð903 90]48 2[644 7[9 * * * * * * * 0 * * * 0 * * * * * * * * * * * *84Ð911 99]47 2[604 7[9 2 * * 0 * * * * * * * * * * * 0 * * * * * * * *83Ð929 99]04 2[563 7[9 1 * * * * * * 0 * * * * * * * * * * * * * * * *83Ð926 91]39 2[503 6[0 * * * * * * * * * * * 2 * * * * * * * * * * * *
83Ð934 99]07 2[485 6[8 0 * * * * 0 * * * * * 0 * * * * * * * * * * * *83Ð941 99]30 2[448 6[9 * * * * * * * * * * * * * * * * * * * * * * * *83Ð959 90]96 2[405 7[9 0 * * * * * * * * * * * * * * * * * * * * * * *83Ð957 99]11 2[362 7[9 * * * * * * * * * * * 0 * * * * * * * * * * * *83Ð964 99]31 2[323 6[9 0 * * * * * * * * * * 0 * * * * * * * * * * * *
83Ð972 99]44 2[278 7[9 0 * * * * * * * * * * * * * * * * * * * * * * *83Ð989 90]03 2[249 6[9 3 * * 0 * 0 * * * 0 * * * * * * * * * * * * * *83Ð987 90]08 2[293 7[9 0 * * * * * * * * 0 * * * * * * * * * * * * * *83Ð095 99]34 2[146 7[9 1 * * * 0 * * * * * * 0 * * * * * * * * * * * *83Ð002 99]35 2[105 6[9 1 * * * * * * * * * 0 * * * * * * * * * * * * *
83Ð013 99]94 2[049 00[9 0 * * * * * * * * 0 * * * * * * * * * 0 * * * *83Ð020 99]04 2[097 6[9 0 * * * * * * * * * * * * * * * * * * * * * * *83Ð027 90]15 2[954 6[9 0 * * * * * * * * * * 0 * * * * * * * * * * * *83Ð035 99]15 2[905 7[9 * * * * 1 0 * * * * * * * * * * * * * * * * * *83Ð043 99]33 1[855 7[9 * * * * * * * * * * * 1 * * * * * * * * * * * *
83Ð051 99]16 1[804 7[9 1 * * * * * 0 * * * * * * * * * * * * * * * * *83Ð058 12]45 1[617 7[9 0 * * * 0 * * * * * * * * * * * * * * * * * * *83Ð066 99]93 1[707 6[9 0 * * * * 0 * * * * * 0 * * * * * * * * * * * *83Ð073 99]01 1[662 6[9 3 * * 0 0 * * 0 * * 0 * * * * * * * * * * * * *83Ð081 99]00 1[619 7[9 2 0 * * * 0 * * * * * * * * * * * * * * * * * *
83Ð088 91]28 1[495 6[0 0 * * * 0 1 * * * * * 0 * * * * * * * * * * * *83Ð196 99]96 1[508 6[8 2 * * * * * * * * * * 0 * * * * * * * * * * * *83Ð103 99]98 1[461 6[9 * * * 0 * 0 * * * * * * * * * * * * * * * * * *83Ð110 99]32 1[413 6[9 * * * * * 0 * * * * * * * * * * * * * * * * * *83Ð118 99]44 1[358 7[9 2 0 * * * * * * * * * * * * * * * * * 0 * * * *
83Ð126 99]13 1[302 7[9 1 * * 0 0 0 * 0 * * * * * * * * * * * * * * * *83Ð134 99]13 1[246 7[9 2 * * 0 * * * * * * * * * * * * * * * * * * * *83Ð142 99]13 1[290 7[9 * * * * * 0 * * * * * 1 * * * * * * * * * * * *83Ð150 99]91 1[134 7[9 0 * * 0 * * * * * * * 0 * * * * * * * * * * * *83Ð157 99]29 1[084 6[9 0 * * * * * * 0 * * * * * * * * * * * * * * * *
83Ð165 99]99 0[784 7[9 0 * * * * * * 0 * 0 * * * * * * * * * * * * * 083Ð172 04]03 1[973 6[5 3 * * * 0 * * * * * * 0 * * * * * * * * * * * *83Ð174 12]47 0[705 1[383Ð182 99]91 1[907 6[9 0 0 * 0 * * * * * * * 0 * * * 0 * * * * * * * *83Ð290 99]05 0[851 7[9 0 * * * * * * 1 * * * 0 * * * * * * * * * * * *
83Ð298 99]90 0[895 7[9 4 * * * * 1 * 0 * * 0 * * * * * * * * * * * * *83Ð206 99]91 0[740 7[9 4 * * * * 0 * 0 * * * * * * * * * * * * * * * *83Ð213 99]25 0[793 6[9 1 * * 0 * * * * * * * * * * * 0 * * * * * * * *83Ð220 95]05 0[644 6[1 0 * * * 0 0 * * * * * * * * * 0 * * * * * * * *83Ð228 90]36 0[694 6[7 0 * * * * 0 * 0 * * * 0 * * 0 * * * * * * * * *
continued
H[ Kru�`er et al[ : Planetary and Space Science 36 "0888# 252Ð272269
Table 1*continued
Date Time R Dt AC AC AC AC AC AC AC AC AC AC AC AC AC AC AC AC AC AC AC AC AC AC AC AC"h# "AU# "d# 90� 00� 10 20 91� 01 11 21 92 02 12 22 93 03 13 23 94 04 14 24 95 05 15 25
83Ð236 99]09 0[544 6[8 2 * * * 0 * * * * 0 * 0 * * * * * * * * * * * *83Ð243 99]33 0[502 6[9 0 * * * 0 * * * 0 * * * * * * * * * * * * 0 * *83Ð251 99]99 0[203 7[9 0 * * * 0 * * * * * * * * * 0 0 * * * * * * * *84Ð993 90]06 0[418 6[0 * * * * 0 * * * * * * * * * * * * * * * * * * *84Ð901 99]91 0[377 6[8 0 * * * * 0 * * * * 0 * * * * 0 * * * * * * * *
84Ð908 12]46 0[331 7[9 2 * * * 0 * * * * * * * * * 0 0 * * * * * * * *84Ð916 99]93 0[312 6[9 4 * * * * * * * * * * 0 * * * * * * * * * * * 084Ð923 12]48 0[271 7[9 4 * * * * * 0 * * * * * * * * * * * * * * * * *84Ð931 90]17 0[264 6[0 2 * * * * * * 0 * * * * * * * * * * * * * * * *84Ð949 90]92 0[246 7[9 1 * * * * * * * * * * * * * * * * 0 * * * * * *
84Ð947 99]46 0[235 7[9 4 * * * 0 * * 0 0 * * 0 * 0 * * * * * * * * * *84Ð955 99]90 0[239 7[9 6 0 * 0 * * * * * * * 0 * 1 * * * 0 * * * * * *84Ð962 99]30 0[239 6[9 00 * * * 1 * * * 0 * 0 * * * 0 * * 0 0 * * * *84Ð979 90]25 0[235 6[9 6 * * * * * * * * * 0 * * * * * * * * * * 0 * *84Ð977 99]18 0[247 7[9 5 * * * 2 * * * * * * 0 * * * * * * * * * * * 1
84Ð984 99]29 0[262 6[9 8 * 0 * * * * * * * * 0 * * * * * * 0 0 * * * *84Ð092 99]97 0[284 7[9 7 * * * * * * * * * * 1 * * * * * * * * * 0 * *84Ð000 99]99 0[365 7[9 3 * * * * 0 * * * * * * * * * * * * * * * * * *84Ð008 99]04 0[345 7[9 2 0 * * * * * * 0 * * * * * * * * * * * * * * *84Ð016 99]29 0[382 7[9 * * * 0 * * * * * * * * * * * * * * * * * * * *
84Ð024 99]00 0[423 7[9 1 0 * 0 * * * * * * * * * * * 0 * * * * * * * *84Ð031 99]24 0[461 6[9 4 * * * * * * * * * * * * * * * * * * * * * * *84Ð049 99]40 0[508 7[9 0 * * * 0 * * * * * * * * * * * * * * * * * * *84Ð047 90]94 0[556 7[9 1 * * * * * * * * * * 0 * * * * * * * * * * * *84Ð055 90]14 0[607 7[9 0 * * * * * * 0 * * * * * * * * * * * * * * * *
84Ð063 90]39 0[669 7[9 1 * * * * * * * * * * * * * * * * * * * * * * *84Ð071 90]04 0[713 7[9 1 * * * * * * * * * * * * * * * * * * * * * * *84Ð078 90]32 0[761 6[9 * * * 1 0 * * * * * * * * * * * * * * * * * * *84Ð086 90]94 0[816 7[9 * * * * * * * 0 * * * * * * * * * * * * * * * *84Ð193 90]40 0[865 6[9 2 * * * * * * * * * * 0 * * * * * * * * * * * *
84Ð101 99]96 1[921 6[8 1 0 * * 0 * * * * 0 * * * * * * * * * * * * * *84Ð108 99]96 1[971 6[9 0 * * * 2 * * 0 * * * * * * * * * * * * * * * *84Ð115 90]05 1[020 6[9 1 * * * 0 * * * * * * * * * * * * * * * * * * *84Ð122 90]31 1[070 6[9 3 * * * 0 * * * * * * * * * * * * * * * * * * *84Ð139 12]48 1[349 6[8 2 * * * * * * * * * * * * * * * * * * * * * * *
84Ð137 99]38 1[176 6[9 1 0 * * * * * * * * * * * * * * * 0 * * * * * *84Ð144 90]07 1[225 6[9 0 * * * * * * * * * * * * * * * * * * * * * * *84Ð151 90]49 1[274 6[9 0 * * * * * * * * * 0 0 * * * * * * * * * * * *84Ð169 99]08 1[330 6[8 2 * * * * * * 0 * 0 * * * * * * * * * * * * * *84Ð166 99]08 1[378 6[9 0 * * * * * * * * * * * * * * * * * * * * * * *
84Ð173 90]03 1[427 6[9 1 * * * * * * * * * * * * * * * * * * * * * * *84Ð181 99]97 1[481 7[9 0 * * * * * * * * * * * * * * * * * * * * * * *84Ð188 99]16 1[539 6[9 1 * * * 0 * * * * * * 1 * * * * * * * * * * * *84Ð295 90]27 1[576 6[9 2 * * * * * * * * * * * * * * * * * * * * * * *84Ð202 90]27 1[622 6[9 0 * * * * * * * * * * * * * * * * * * * * * * *
84Ð219 92]26 1[679 6[0 2 * * * * * * * * * * 0 * * * * * * * * * * * *84Ð217 90]10 1[720 6[8 0 * * * 1 * * * * * * * * * * * * * * * * * * *84Ð224 91]27 2[035 6[0 * * * * * * * * * * * * * * * * * * * * * * * *84Ð233 02]00 1[826 8[3 0 * * 0 * * * * * * * * * * * * * * * * * * * *84Ð234 99]94 1[830 9[4
continued
H[ Kru�`er et al[ : Planetary and Space Science 36 "0888# 252Ð272 260
Table 1*continued
Date Time R Dt AC AC AC AC AC AC AC AC AC AC AC AC AC AC AC AC AC AC AC AC AC AC AC AC"h# "AU# "d# 90� 00� 10 20 91� 01 11 21 92 02 12 22 93 03 13 23 94 04 14 24 95 05 15 25
84Ð241 90]99 1[874 6[9 0 * * * * * * * * * * 0 * * * * * * * * * * * *84Ð259 90]04 2[924 7[9 0 * * * 0 * * * * * * * * * * * * * * * * * * *
Impacts "counted# 124� 06� 0 07 39� 29 4 36 2 8 5 52 9 3 2 01 9 2 1 4 9 2 9 3Impacts "complete data# 124 06 0 07 39 29 4 36 1 8 5 52 9 3 2 01 9 2 1 4 9 2 9 3All events "complete data# 57065 2565 0 07 627 29 4 36 2 8 5 52 0 3 2 01 9 2 1 4 9 2 9 3
� Entries for AC90\ AC00 and AC91 are the number of impacts with complete data[ Due to the noise contamination of these three categories thenumber of impacts cannot be determined from the accumulators[ The method to separate dust impacts from noise events in these three categorieshas been given by Baguhl et al[ "0882#[
mass error factor "MEF# are given in the last columns[For VEF× 5\ both velocity and mass values should bediscarded[ This occurs for 37 impacts[ No intrinsic dustcharge values are given "see Svestka et al[\ 0885 for adetailed analysis#[
3[ Analysis
The positive impact charge measured on the ion collec!tor\ QI\ is the most important impact parameter deter!mined by the dust instrument because of its relativeinsensitivity to noise[ In Fig[ 3 we show the distributionof QI for all dust particles detected between 0882Ð84[ Ionimpact charges have been detected over the entire rangeof six orders of magnitude in impact charge that can bemeasured by the dust instrument[ About 0) of allimpacts are close to the saturation limit of QI ½ 09−7 Cand may thus constitute lower limits of the actual impactcharges[ The impact charge distribution is reminiscent ofthree individual particle populations] small particles withimpact charges QI ³ 09−02 C "AR0#\ intermediate par!
Fig[ 3[ Distribution of the impact charge amplitude QI for all particlesdetected between 0882Ð84[ The solid line indicates the number ofimpacts per charge interval\ and the dotted line shows the cumulativepercentage[ Vertical bars indicate the zn statistical error[
Fig[ 4[ Channeltron ampli_cation factor A � QC:QI as a function ofimpact charge QI for all particles detected between 0882Ð84[ The solidlines denote the sensitivity threshold "lower left# and the saturation limit"upper right# of the channeltron[ Squares indicate dust particle impacts[The area of each square is proportional to the number of events included"the scaling of the squares di}ers from that used in Paper III#[ Thedotted horizontal line shows the mean value of the channeltron ampli!_cation A � 1[0 for ion impact charges 09−01 C ³ QI ³ 09−00 C[
ticles with 09−02 C¾QI ¾ 2×09−00 C "AR1 and AR2#and big particles with QI × 2×09−00 C "AR3 to AR5#[The intermediate particles are mostly of interstellar originand the big particles are interplanetary particles detectedclose to the ecliptic plane "Gru�n et al[\ 0886^ see alsoSection 4#[ The small particles occur mostly over theSun|s polar regions and are attributed to a populationof interplanetary b!meteoroids at high ecliptic latitudes"Baguhl et al[\ 0884b^ Hamilton et al[\ 0885#[
The ratio of the channeltron charge QC and the ioncollector charge QI is a measure of the channeltron ampli!_cation A[ The channeltron ampli_cation is an importantparameter for dust impact identi_cation "Paper I#[ In Fig[4 we show the charge ratio QC:QI as a function of QI forthe nominal high voltage of 0039 V "HV�2#[ The meanampli_cation determined from particles with 09−01
C¾QI ¾ 09−00 C is A¹ 1[0[ This is very close to thevalue obtained in Paper III for the _rst two years of the
H[ Kru�`er et al[ : Planetary and Space Science 36 "0888# 252Ð272261
mission "A¹ 1[1#[ Therefore\ the channeltron does notshow any detectable aging during the more than _ve yearsof the Ulysses mission[
Figure 5 shows the masses and velocities of all dustparticles detected between 0882Ð84[ As in the earlier per!iod "0889Ð81^ Paper III#\ velocities occur over the entirecalibrated range from 1Ð69 km:s[ The masses vary over09 orders of magnitude from 09−5 gÐ09−05 g[ The meanerrors are a factor of 1 for the velocity and a factor of 09for the mass[ The clustering of the velocity values is dueto discrete steps in the rise time measurement but thisquantization is much smaller than the velocity uncer!tainty[ For many particles in the lowest two amplituderanges "AR0 and AR1# the velocity had to be computedfrom the ion charge signal alone which leads to the stri!ping in the lower mass range in Fig[ 5 "most prominentabove 09 km s−0#[ In the higher amplitude ranges thevelocity could normally be calculated from both the tar!get and the ion charge signal\ resulting in a more con!tinuous distribution in the mass!velocity plane[ Impactvelocities below about 2 km:s should be treated withcaution because anomalous impacts onto the sensor gridsor structures other than the target generally lead to pro!longed rise times and hence to unnaturally low impactvelocities[
4[ Discussion
Most of the time from January 0882ÐDecember 0884\Ulysses was at high ecliptic latitudes far away from theecliptic plane[ The dust impact rate detected by theUlysses dust sensor in this period is displayed in Fig[ 6[The highest overall impact rate was detected around the
Fig[ 5[ Masses and impact velocities of all impacts recorded with theUlysses sensor between 0882Ð84[ The lower and upper solid lines indi!cate the threshold and the saturation limit of the detector\ respectively\and the vertical lines indicate the calibrated velocity range[ A sampleerror bar is shown that indicates a factor of 1 uncertainty for the velocityand a factor of 09 for the mass determination[
ecliptic plane crossing which occurred on 01 March 0884"at 0[2 AU from the Sun#[ The maximum impact rate ofparticles in the three highest ion amplitude ranges "AR3to AR5# coincides with the highest overall impact rate"upper panel of Fig[ 6#[ These impacts are attributed tointerplanetary particles on low inclination orbits "Gru�net al[\ 0886#[ These are the impacts with QI × 09−09 Cshown in Fig[ 3[ The impact rate of particles in the lowestamplitude range "AR0# increased gradually since mid0882\ reached its maximum at the ecliptic plane crossingin March 0884 and decreased later[ Although the impactrate reached its maximum during a short time aroundthe ecliptic plane crossing\ the majority of these smallparticles has been detected during the much longer timeinterval when Ulysses was at high ecliptic latitudes[ Theyare attributed to a population of small interplanetaryparticles on escape trajectories from the solar system"Baguhl et al[\ 0884^ Hamilton et al[\ 0885#[
The impact rate of particles in the intermediate ionamplitude ranges AR1 and AR2 was relatively constantduring the 0882Ð84 period[ It dominated the overallimpact rate until early 0883\ i[e[\ outside about 2[4 AU
Fig[ 6[ Impact rate of dust particles detected with the Ulysses dustsensor as a function of time with the ecliptic latitude of the spacecraftindicated at the top[ Upper panel] the upper solid line shows the totalimpact rate\ the dotted line the impact rate of small particles "AR0# andthe lower solid line the rate of big particles "AR3ÐAR5#[ Note that arate of about 0[7×09−6 impacts per second is caused by a single dustimpact in the averaging interval of about 69 days[ Lower panel] inter!mediate particles "AR1 and AR2\ solid line#[ A model for the rate ofinterstellar particles assuming a constant ~ux is superimposed as adashed line[
H[ Kru�`er et al[ : Planetary and Space Science 36 "0888# 252Ð272 262
Fig[ 7[ Rotation angle vs time for all particles detected between 0882Ð84 for which complete information is available[ Plus signs indicateparticles with impact charge QI ³ 7×09−03 C\ squares those withQI − 7×09−03 C[ The contour lines show the sensitive area of the dustsensor for particles approaching from the interstellar upstream direction"levels of 0\ 299\ 599 and 899 cm1 detector area are shown#[ Most of thelarger QI particles came from directions consistent with the interstellarupstream direction[ The biggest particles in the highest amplitude rangeswhich are of interplanetary origin are not shown separately here becauseonly very few of them were detected "cf[ Table 1# and they cannot beseparated from interstellar particles by directional arguments[ passageover the Sun|s south polar region occurred in October 0883\ eclipticplane crossing in March 0884\ and passage over the Sun|s north polarregion in August 0884[
from the Sun[ Impacts in these ion amplitude ranges aremostly due to interstellar particles "see also Fig[ 7 andGru�n et al[\ 0882^ Baguhl et al[\ 0884#[ Figure 6 alsoshows the expected impact rate of interstellar particlesassuming that they approach from the direction of inter!stellar helium "Witte et al[\ 0885# and that they move onstraight trajectories with a relative velocity of 15 kms−0 through the solar system[ This assumption meansdynamically that radiation pressure cancels gravity forthese particles "b�0# and that their Larmor radii arelarge compared with the dimension of the solar system[Both assumptions are reasonable for particles withmasses between 09−02Ð09−01 g which is the dominant sizerange measured for interstellar particles "e[g[\ Gru�n et al[\0886#[ The dust particle ~ux is independent of heliocentricdistance in this simple model\ which gives relatively goodagreement with the observed impact rate[ The variationpredicted by the model is caused by changes in the instru!ment|s viewing direction with respect to the approachdirection of the particles and changes in the relative vel!ocity between the spacecraft and the particles[ After theecliptic plane crossing the rate of interstellar particlesexpected from the model is signi_cantly higher than theone observed[ A detailed dynamical model "Landgraf\0887# for the motion of interstellar particles in the inter!
planetary magnetic _eld gives better agreement with theobserved impact rate\ especially after 0885[
The sensor orientation at the time of a particle impact"rotation angle# is shown in Fig[ 7[ The detector|s sen!sitive area for particles approaching from the interstellardirection is superimposed[ The bigger particles "squares\impact charge QI − 7×09−03 C# are clearly concentratedtowards the interstellar direction[ They have beendetected with a relatively constant rate during the wholethree!year period "Fig[ 6#[ Only a few small particles"crosses\ impact charges QI ¾ 7×09−03 C# have beendetected and they cluster above the Sun|s polar regions[The particles with the highest ion amplitude ranges"AR3ÐAR5# are not distinguished in this diagrambecause they cannot be separated from interstellar par!ticles by directional arguments[ They have to be dis!tinguished by other means "e[g[\ mass and velocity#[Furthermore\ their total number is so small that theyconstitute only a small {contamination| of the interstellarparticles in Fig[ 7[ In the ecliptic plane at 0[2 AU\however\ interplanetary particle ~ux dominates overinterstellar ~ux by a factor of about 2 "in number#[
Streams of tiny dust particles originating from the Jov!ian system have been _rst detected with Ulysses and laterwith Galileo out to 1 AU from Jupiter "Gru�n et al[\ 0882\0885#[ During the time period from 0882Ð84 consideredhere\ Ulysses was more than 1[4 AU away from Jupiterwhich makes a signi_cant contribution of Jovian duststream particles in the present data set very unlikely[Analysis of the particles| trajectories and their interactionwith the interplanetary magnetic _eld "Zook et al[\ 0885#showed that the velocities are about 299 km:s and theparticles are about 09 nm in size[ These values are farbeyond the calibrated range of the dust sensors givenabove and\ in principle\ one cannot exclude that the dataset presented in this paper contains at least a fraction ofparticles for which the masses and velocities inferred fromour calibration are wrong[ Recent analyses of the inter!planetary "Gru�n and Staubach\ 0886# and interstellarpopulations "Landgraf\ 0887#\ however\ are consistentwith the calibrated velocities and masses of the particlesin the new 0882Ð84 data set[ Given the present knowledgeabout the particles| dynamics\ the velocities and massesstated in Papers II and III for the stream particles arenot correct[ Future investigations will address possiblecontributions of particles beyond the calibrated range ofthe dust instruments in the complete Ulysses and Galileodata sets\ not only close to Jupiter where the dust streamshave been detected[
Acknowledgements
This work has been supported by the Deutsche Agen!tur fu�r Raumfahrtangelegenheiten "DARA#[
H[ Kru�`er et al[ : Planetary and Space Science 36 "0888# 252Ð272263
Tab
le2
Raw
data
]No[
\im
pact
tim
e\C
LN
\AR
\SE
C\I
A\E
A\C
A\I
T\E
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VD
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P\E
CP\C
CP\P
CP\H
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ted
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PC
CP
PC
PH
VR
LO
NL
AT
DJu
pR
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SL
ON
SL
AT
VV
EF
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858
82Ð9
9097
]92
00
097
63
098
029
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99
09
99
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4[95
519
059[
5−
04[5
4184
[838
142
3003
[00[
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3=0
9−03
09[4
869
82Ð9
9298
]95
22
097
1914
005
55
90
329
09
99
02
4[95
066
059[
5−
04[7
4216
[588
888
888
817
[90[
54[
8=0
9−02
5[9
860
82Ð9
9309
]45
21
019
0119
56
55
90
279
09
99
02
4[94
857
059[
5−
04[7
4231
[456
148
1223
[00[
84[
1=0
9−03
09[4
861
82Ð9
9494
]44
21
018
0904
005
65
90
259
09
99
02
4[94
700
059[
5−
04[8
4242
[579
152
0032
[40[
87[
4=0
9−04
09[4
862
82Ð9
9402
]32
22
138
0811
006
65
90
309
09
99
02
4[94
621
059[
5−
04[8
4248
[188
888
888
810
[90[
57[
1=0
9−02
5[9
863
82Ð9
9704
]25
21
597
028
88
89
09
90
99
90
24[
9496
205
9[6
−05
[043
94[5
888
888
888
10[9
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6[1
=09−
035[
986
482
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19]9
49
107
88
19
804
040
928
290
99
90
24[
9308
005
9[6
−05
[243
55[7
057
211
−52
03[0
0[8
4[7
=09−
0309
[486
582
Ð901
12]2
39
001
86
49
604
040
99
90
99
90
24[
9305
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72
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42
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82
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59
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812
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22
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44
90
369
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317
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0961
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90
443
29
503
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200
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9569
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292
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370
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21
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45
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319
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309
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323
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7−
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161
423
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1992
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90
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1000
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21
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9254
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651
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483
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315
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62
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62
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49
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82
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59
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7245
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92
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292
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21
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328
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9−
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0807
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90
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76
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313
09
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2[62
543
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7−
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8867
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155
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0=0
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23
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543
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7−
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8867
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142
1511
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7=0
9−01
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cont
inue
d
H[ Kru�`er et al[ : Planetary and Space Science 36 "0888# 252Ð272265
Tab
le2*
cont
inue
d
No[
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LN
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29
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H[ Kru�`er et al[ : Planetary and Space Science 36 "0888# 252Ð272267
Tab
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cont
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d
No[
IMP[D
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LN
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SEC
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H[ Kru�`er et al[ : Planetary and Space Science 36 "0888# 252Ð272279
Tab
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cont
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d
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H[ Kru�`er et al[ : Planetary and Space Science 36 "0888# 252Ð272271
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