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7/26/2019 N. a. Kozyrev - Spectral Evidence of Outflow of Molecular Hydrogen in the Region of Aristarchus
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SPECTRAL EVIDENCE OF OUTFXOW OF MOLECULAR HYDROGEN N THE
REGION OF ARISTARCHUS i
N A Kozyrev
ABSTRACT. Sp ec tr al obs erv ati ons of th e c r a t e r Ar ist are hus
du ri ng November and December 1961 showed a c om par ati ve ly s t a b l e
outf low of gas nea r i t s cen te r .
The emission band 4634 f A
wi th a sharp red border and weak emission i n t he orange-red
s p e c t r a l r e gi o n
were detec ted .
These da ta a re ev idence th a t th er e was an ou t f low of
molecular hydrogen of t h e fumarole type of Eart h volcanoes,
I n ord er t o c l a r i f y th e luminescence glow of th e Moon i n 1955,
a
photo-
me tr i c comparison was made of th e spe ct ra of d if fe re nt o bj ec ts on th e Iunal:
su r f a ce and th e so l a r spect ru m [ I ] .
The spectrograms were obtained on a
50 inch
re f l ec to r o f th e Crimean Ast rophysica l Observa tory , us ing a spec t rograph having
a l i n e a r d i sp e r s io n of ab o ut
3
t
mm
n ea r
H
P a r t i c u la r a t t e n t i o n
w s
i n t h e s p e c t r a of o b j e c t s on t h e L unar s u r f a c e and i n t h e s o l a r s p e c t r m .
m r
was a s i g n i f i c an t d i f f e r en ce i n th e co n to ur s o f th ese l in es and th e co n to ur s of
th e so la r spect ru m o n ly i n th e spect ru m o f th e Ar i s t a r ch u s c r a t e r .
n
t h e Aris
t a r ch u s spect ru m, th e l in e s w e r e n ar ro wer th an i n t h e s o l a r spect ru m,
It
thus
f o l l o w s t h a t t h e r e
i s
a lumin escence g lo w i n - th e Ar i s t a r ch u s c r a t e r
which
closes
t h e l i n e c on to ur s,
A photometr ic s tudy showed th a t t h i s g low ex is ts
i n the
narrow wave port ion of the spectrum a t 4000 A
Pn
a d d i t i o n , t h e r e w a s a
second, weaker reg ion of luminescence between 4400 and 4100 A
Numbers i n t h e marg in d es ig n a te p ag in a t io n i n o r ig in a l f o r e ig n t e x t
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This luminescence of th e Ar is ta rch us c r a t e r was most c l ea r l y apparen t after
a f u l l Moon. However, a t t h e same phase bu t i n di f f e r e n t months, th e Busaineseence
br ig h tne ss was f a r from th e same. These f luc t ua t ion s i n b r igh tnes s had no con
n e c t io n w i th s o l a r a c t i v i t y . Th e refo re , t h e q u es t io n a r i s e s o f wh e th er th ey m
n o t b e e x pl a in e d by c ha ng es i n t h e a c t i v i t y o f t h e c r a t e r i t s e l f .
Such
an
ex
p lan a t io n may b e v a l id , i f a s i g n i f i c an t p o r t io n o f t h e o bserved emiss ion s i s
caused, not by luminescence of s o l i d rocks,
bu t by luminescence of gas
outflows
from th e Ar i s t a r ch u s c r a t e r ,
I n o r d e r t o s t ud y t h i s prob le m, i n
November-
December, 1961, a new se r i e s o f s p e c t r a l o b se rv a t io n s o f t h e Ar is t a r ch u s
crater
was performed on a 50-inch r e f l e c t o r of t h e Crimean Observatory.
, I n 1 96 1, s p e c t r a of t h e A r i s t a r c h u s c r a t e r w e r e obtained on a different
sp ec tro g rap h wi th a sma l l d i sp e r s io n , o n th e o rd e r of 15 0 a t m n ea r H
.
Y
The sp ec tr a were recorded wit h a wide
s l i t
thus making i t p o s s i b l e t o
have
the
sp ec t ru m o f th e c r a t e r and th e s p ec t r a o f i t s sur roundings a t th e same
time A t
t h i s t ime, the photometr ic p rocess in g of t he sp ec t ra ob ta ined was concluded by
comparing th e spect rum of th e ob jec ts s tu d ie d wi th th e spec t rum of the su r ro md -
in gs , and no t wit h th e so l a r spectrum. On November 30, i n th e mornirng, t he Moon
was in th e l a s t q u a r t e r . Spect ro grams o f th e Ar i s t a r ch u s c r a t e r and
i t s
selrromd-
i n g s
were
obta ined during th e nightt i me i n November on th e fol low ing days
25-26 27 28 29
-30 and i n December:
1
2 2 3 .
On the se nig ht s, a la rg e number of spectrograms were made of detai ls
i n the
Ar is t a r c h u s and Herod otus c r a t e r s , t h e Sch ro e te r Va l ley , i n d iv id u a l c r a t e r s ,
and ot he r de t a i l s of th e Wood Spot . A group of emiss ion bands, beginning
abr upt ly and passing f ur th e r toward the short-wave end of t h e spectrum, was
even
no ti ce ab le without photometr ic comparison on ce r t ai n spectrograms obtaine d
in
t h e v e ry cen t e r of th e Ar i s t a r ch u s c r a t e r , between
H
and
N .
Fig u re
I shows
f
th e re s u l t s der ived f rom photometr ic p rocess ing of spec trograms of t h i s s pe c t r a l
region.
The lo g a r ith ms o f t h e r a t io s b etween th e b r ig h tn ess o f th e
Aristalrchus
ce nt er spectrum and th e br i ght ne ss used f o r comparing th e spectrum of one of the
a d ja c en t d e t a i l s o f t h e l u n a r s u r f a c e a r e p l o t t e d a lo ng t h e o r d i n a t e axis
Spect rogram s f o r November
5
and
7
were each measured wit h res pe ct t o t w o
dif-
fe ren t compar ison spec t ra .
A s m y
b e seen f r o h F ig u re 31 the emiss ion
may be
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Figure
1
Emiss ion observed i n th e bl ue por-
t i o n o f t h e sp ec tr um f o r t h e c r a t e r
Ar i s t a rchus . One d iv i s ion on t h e ve r t i c a l
s c a l e equal s 0.10 of t h e common loga rith m of
br igh tness .
observed on two spec t rogram
obtained on December 3 The
sharp emiss ion boundag near
t h e red end of t he sp ee t r m
and
i t s
cl ea rl y marked st ru c-
t u r e d e f i n i t e l y e s t a b l i s h t h e
gaseous nature of this emission,
Important confirmation
of this
conclus ion
i s
t h e fact that i n
photographs taken December 3,
th e emission bands observed
above th e br ight
central pore
t i o n of t h e c r a t e r protrude I0
somewhat into the
s p e c t r u m
of
th e shade thrown
out
by t h e
Eas te rn s i de o f t he c ra t e r edge.
t
thus fol lows th a t th e emiss ion source
ex-
t e n ds t o a c e r t a i n h e i g h t ab ov e t h e c r a t e r s u r f a c e .
The obse rva t ions i nd i ca t e t ha t t he re
i s
a c t u a l l y l i b e r a t i o n o f g as es i n t h e
c e n t e r of t h e A r i s t a r ch u s c r a t e r , more p r e c i s e l y , i n
i t s
ce n t ra l peak ,
The a@-
t i v i t y of such processes cannot be cons tant .
t i s
v e r y p o s s i b l e t h a t t h e sb-
s e r v a t i o n of e mi ss io n s c l o s e t o t h e l a s t q u a r t e r ,
i . e . ,
when t h e Sun
i s
&ove
t h e c r a t e r ,
i s
not acc id en t a l , and t ha t t he ou tf l ow s f gases
i s
f a c i l i t a t e d
by hea t in g by s o la r rays of t h e cor responding c ra t e r r eg ions .
t i s now
i n t e r -
e s t i ng t o c l a r i fy t h e chemica l na tur e s f t he gases p roduc ing t he observed
emission.
Figure 1 shows t h a t th e s harp emission boundary from th e red end
of
the
spec trum has a wavelength between 4630 and 4638 1
On t h e av era ge = 4634
fo r t h i s boundary. The t ab l e s s f molecu la r sp ec t r a do no t i n d i c a t e
t h e
exis-
ten ce of a band with a red edge of t h i s wavelength. Bands of t h e malecuies
M
o r Z r O ar e more su i t ab le . However, t h e behavior of ot he r bands of th es e mole-
cules completely re f ut e such
a
p o s s i b l e i d e n t i f i c a t i o n .
There
i s
s t i l l
one
o t h e r i n t e r e s t i n g p o s s i b i l i t y r e l a t e d t o t h e form of t h e E a s te r n hyd rog en
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Fig u re
2
Comparison of emission observed i n t he Arista rehu s
crater
( so l id l i n e ) w i th th e emissio n sp ec trum of mo lecula r hy-
d ro gen o b ta in ed wi th th e same d i sp e r s io n (dash ed l i n e , d r am i n
a n a r b i t r a r y s c a l e ) . One d i v i s i o n on t h e v e r t i c a l s c a l e
equals
0.05 of t h e common br ig ht ne ss l oga rith m.
spectrum, i . e . t h e sp ec trum o f th e
M
mo lecu le s f o r sma l l d i sp e r s io n s .
Thhe
b r i g h t e s t l i n e s of t h i s complex spect ru m are concent rated i n two wavelength
reg io n s
-
h e reddish-orange and th e blue .
The blue region of H m i s s i o n
b eg ins w i th
a
p a r t i c u l a r l y b r i g h t l i n e h av ing
a
wavelength a t
4634 A This
s
t h e main l i n e o f th e s in g u le t sy s tem 3d C - 2pvC of hydrogen vapor.
Because o
t h i s l i n e , f o r s m a l l d i s p e r s i o n s t h e b l u e s p e c t r a l r e gi o n of
H
w i l l appear as
a wide band with a sharp red edge.
For purposes of bet ter comparison
i n
t h e
laboratory, we recorded and measured the
H
spectrum obtained by a sp ec t ro -
graph,
s f a lm o st p r e c i s e l y t h e same d i s p e r s i on a s t h a t us ed t o o b t a i n
the
spec
t ru m o f t h e Ar i s t a r ch u s c r a t e r .
The dashed l i n e s i n Figure 2 show the r e s u l t s
of measuring t h i s l abor a tory spec t rum of H
The so l id l ine shows the supple-
mentary emissions o f t he Ar is ta rc hus c ra te r measured over the e n t i r e spec t r .m,
I n t h e b l u e s p e c t r a l re gi on , t h i s
curve i s obta ined by averag ing th e da t a i n
Fig u re
1
The dashed and s o l id l i n e s c lose ly co inc ide . With respec t
t o the
redd ish-orange sp ec t r a l reg ion , where th er e
i s
in te ns e emission of
H
rno8ecules
(pr imar i ly th e t r i p l e t l i n e s s f o rtho-hydrogen) , pho tometr ic measurements
re-
v e a l a weak glow of t h e Ar is ta rc hus c ra te r .
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t i s impor tant t o note t ha t both thes e emiss ions a re bounded by approxi-
l
mately the same wavelength region.
The la c k of agreement between t h e patter n.
o f t h e s o l i d l i n e and t h a t o f t h e dashed l i n e must p r im ar i l y p e r t a in t o the
small
d i s p e r s io n and t h e o ve rexp os ur e o f p h o to g r ap h s in t h i s s p e c t r a l region
t
i s o u r op in io n t h a t t h e m a te r i a l i n F ig u re
2
l e ad s t o t h e r e l i a b l e c s ncLu sion
th a t t h e g a s o u tf lo w in g f rom th e A r i s t a r ch u s c r a t e r i s molecular hydrogen,
Usually, t h e atomic hydrogen spectrum e x i s t s along wit h th e seccandaqr
hydrogen spectrum under lab ora to ry c ond itio ns.
In the spectrum of the
Aris tarc hus cr at er , sp ec ia l measurements d id not rev eal any dif f ere nce s between
th e Balmer l i ne s and t he Balmer l i n e of th e spec t rum fo r
i t s
s u r r o m d i n g s ,
Thus,
i t
may b e assumed t h a t no si g n if ic a n t amount sf atomic hydrogen s
pro
duced i n the ex ci ta t i on of molecular hydrogen outf lowing from the cen ter of the
A r i s ta r ch u s c r a t e r . T hi s r ep r e s en t s a v e ry imp o rt an t ch a r ac t e r i s t i c
sf hydrogen
glow pr oc es se s on t h e Moon. t must be noted th a t i t i s extremely d i f f i c u l t to
f in d a cor rec t exp lana t ion f o r t h i s g low mechanism, due t o th e la rg e = c i t a t i o n
energ ie s o f
H
molec ules. The observed out flow of molecular hydrogen
cmnot
be
the r es u l t o f pho tod is soc ia t ion o f wate r vapor , s in ce on ly the fo rmat ion o f
and OH
i s
i n t r i n s i c t o t h i s p r oc es s.
H
can be produced by th e ph otsdissoc ia-
2
t i on o f o t her molecu les . t must th er ef or e be concluded t h a t molecular hydrogen
i s
produced d i r ec t l y i n t he i n t e r i o r o f th e Moon.
t
can t h en accm u la t e t h e r e ,
Th is conc lus ion regard ing ex is tence o f molecu lar hydrogen i n th e in te r i o r
of
the
Moon agree s wit h t h e exi ste nc e of l o c a l accumulations of hydrogen
i n
t h e E a r th ' s
c r u s t .
The
impor tan t ro le o f molecu la r hydrogen ou t f low in th e vo lc mi c
pra-
cesses on the Ear th
i s
w e l l known.
The observa t ions d escr ibed her e show tha t comparat ively s t ab le gas outflows
of t h e fumarole type of our t e r r e s t i a l volcanoes ex i s t
on t h e Moon, i n a d d i t i o n
t o spontaneous volc an ic proce sses observed on :~ovember
3
1958 and October 23,
1959 i n t h e A lf on s c r a t e r . The fu m ar ol e f i e l d was l o ca t ed t o t h e ea s t
of
t h e
ce n t ra l peak i n th e Ar i s ta rc hus c ra te r , and was on the o rder of 1 -2 i n s i z e ,
i , e . 2 4 km. C lo se t o t h i s f i e l d (on t h e e a s t e r n edge of t h e A r i s t a r A u s
c r a t e r an d
a t
t h e apex of t h e Sch roeter Val ley) Greenacre and Barr a t the
Lowell Observatory
on
30 October
1 9 6 3
observed two re gi on s which were reddish-
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orange i n co lo r and l a s t ed f o r
20
minutes [ 2 ]
During these observations,
the
Ar is ta r chus c r a t e r was c los e to t he t e rmina to r fo r 2.5 days before
the f u l l
Moon.* The br ie f appearance of th e br ig ht c ol or i s def in i t e ly caused
by
the
outflow of gas es whose glow was p a rt ic ul a rl y apparent on th e background of t h e
l u n a r su r f a c e c l o se t o t h e t e r mi n at o r. The almost simultaneous
appearance
of
gases i n two reg ions separ ated by 35 sm
(5
m in ut es e a r l i e r i n t h e S c hr o et e r
Valley) could have been th e re s ul t of a si n g le deep process.*
Thus,
these
new
observat ions of Greenacre and Barr confi rm the g rea t volcanic a c t iv i t y
of the
Ar is t a r chus c r a t e r r eg ion.*
In conclusion, i t must be pointe d ou t t h a t t h e enigma of t h e Ar i s t a r chus
cr a t er has been f a r f rom solved by thes e observat ions .
The question
s t i l l
of th e Ar i s ta r chus c r a t e r .
In ge nera l , was t h i s luminescence of
a s o l i d
surface
o r was th e luminescence discovered i n 1955, which close d t he contours
o
t h e
B
and
K
l i ne s , en t i r e ly th e luminescence o f ce r t a in gases out f lowing from t he
crater i n t e r i o r which
are
s t i l l
unknown?
Tra ns lat or s Note:
Next
l i n e d el et ed
s
i n di c at e d i n o r i g i n a l
text
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