Cálculo de sistema de alimentación para la biela

T he s tra tig ra p h ie c o n c lu sio n s, b a se d on th e o b se rv a tio n s p re s e n te d a b o v e fro m G u in e v e re an d S e d n a P ia n itia e , are su m m arised below . S tratig rap h ie co rre latio n ch arts fo r V31 and V19 are shown in Figures 3.42 and 3.43 respectively.

1. T he oldest m aterials in the area are in terp reted as T essera and deform ed plains, but this does not im ply all the outcrops are the sam e age. B oth units are em bayed by lineated and m o ttled , and re g io n a l p lain s, fo r in stan ce tesse ra in the area 40^ N 356® E (F ig u re 3.14). H ow ever, the age o f tessera and defo rm ed p lain s u n its re la tiv e to one a n o th e r c a n n o t be e s ta b lis h e d and a c o n sid e ra b le tim e p e rio d m ay e x ist b e tw ee n the fo rm a tio n o f different outcrops of these units (see discussion below).

2. T he lin e ate d and m o ttled p lain s are in te rp re te d to rep re se n t re la tiv e ly old p lain s m aterials w hich have ex p erien c ed m u ltip le phases o f deform ation. The m aterials are deform ed by at least two p h ases o f w rinkle ridges one o f w hich is restricted to this unit. F u r th e r m o r e , rid g e b e lts w h ic h do n o t d e fo rm y o u n g e r surrounding m aterials are observed. O ther sets o f d efo rm atio n not re p re se n te d in yo u n g er p lain s m aterials are o b serv ed . T he tim e d u ratio n rep re se n te d by the lin eated and m o ttled p lain s is n o t clear.

Plains Materials

Tessera

Materials Coronae Materials Edifice Flow Materials

gpr

gph

g p l m

pd

Nissaba Idem-Kuva Silvia Benten materials materials materials materials

Heng-o/Beltis materials hpm ikpr cnf2 c n f l bef bO bf2 hvc2 hvc3 hvcl VC

Figure 3.42 Unit Correlation Chart for units of V31 Sif Mons Quadrangle. The chart is based on unit observations soley from the V31 quadrangle.

UJ Os

Plains Materials

Tessera

Materials Coronae Materials Edifice Flow Materials Flow materials

Other coronae materials Idem-Kuva materials Nissaba materials m eu ikpr nf4 nf2 nfl nO cnf2 npr s p i m sph spr vc

Figure 3.43 Unit Correlation Chart for units of V19 Sedna Planitia Quadrangle. The chart is based on unit observations soley from the V19 quadrangle, m and p show the position of Mesca and Purandi Coronae which have no flow materials associated with them.

U) -c

3. T he reg io n al and hom ogeneous p lain s em bay the m ottled and lin e ate d p lain s. H om ogeneous p lain s are ty p ic ally em b ay ed and hence predate the m ore extensive reg io n al p lain s. B oth units are deform ed by a younger series o f w rinkle rid g es and ridge belts than those which deform the lineated and mottled plains.

4. T he form ation o f edifice fields is considered to have occurred o v e r a re la tiv e ly long p erio d o f tim e. E d ifice field s p re- and p o s td a te re g io n a l p la in s m a te ria ls , c o ro n a e and la rg e sh ie ld volcanoes.

5. P rom inent flow m aterials from large shields (e.g. S if and G ula M o n te s), c o ro n a e (e.g . B e n te n , Id e m -K u v a ) an d g re a t flo w m a te ria ls (N eago F lu c tu s) are ty p ic a lly su p e rim p o se d on the re g io n a l p la in s u n its. T he w rin k le rid g e s w h ich d e fo rm the hom ogeneous and regional plains m aterials also deform the above flo w m a te ria ls lo c a lly . W h ile flo w m a te ria ls a sso c ia te d w ith c o ro n a e are ty p ic a lly young (su p e rim p o sed on re g io n a l p la in s m a te ria ls ), som e c o ro n a e in V31 show p ro tra c te d h is to rie s (C h a p te r 4), w ith in itia l sta g e s p o s td a tin g re g io n a l p la in s emplacement.

6. In the study area, approxim ately 40% o f m aterials can be traced to a source (edifice fields, coronae, large shield v o lcan o es etc.). These landforms are of different ages.

7. T he y o u n g est m ateria ls are d e p o sits a sso c ia te d w ith im p a ct c ra te rs. T he c ra te r d en sity w ith in the m ap p in g q u a d ra n g les is sim ila r to th at c alcu late d fo r the w hole p lan et. A stra tig rap h ie relation cannot be estabhshed between individual craters.