Martian atmospheric disturbances from orbital images and surface pressure at Jezero Crater, Mars, during Martian Year 36

Ma ian A mosphe ic Dis u bances F om O bi al Images
and Su ace P essu e a Jeze o C a e , Ma s, Du ing
Ma ian Yea 36
A. Sánchez‐La ega
1
, E. La sen
1
, T. del Rio‐Gaz elu u ia
1
, J. He nández‐Be nal
2
,
I. O dóñez‐E xeba ía
3
, R. Hueso
1
, B. Tanguy
4
, M. Lemmon
5
, M. de la To e Jua ez
6
,
G. M. Ma ínez
7,8
, A. Mungui a
1
, J. A. Rod íguez‐Man edi
8
, A.‐M. Ha i
9
, J. Pla‐Ga cía
8
,
D. Toledo
10
, and C. Newman
11
1
Escuela de Ingenie ía de Bilbao, Uni e sidad País Vasco, UPV/EHU, Bilbao, Spain,
2
Labo a oi e de Mé eo ologie
Dynamique, So bonne Uni e si é, Pa is, F ance,
3
Plane a io de Pamplona, Pamplona, Spain,
4
LESIA, Obse a oi e de
Pa is, Meudon, F ance,
5
Space Science Ins i u e, College S a ion, TX, USA,
6
Je P opulsion Labo a o y, Cali o nia Ins i u e
o Technology, Pasadena, CA, USA,
7
Luna and Plane a y Ins i u e, Hous on, TX, USA,
8
Cen o de As obiología (INTA‐
CSIC), Mad id, Spain,
9
Finnish Me eo ological Ins i u e, Helsinki, Finland,
10
Ins i u o Nacional de Técnica Ae oespacial,
INTA, Mad id, Spain,
11
Aeolis Resea ch, Chandle , AZ, USA
Abs ac We p esen a s udy o a mosphe ic dis u bances a Jeze o C a e , Ma s, using g ound‐based
measu emen s o su ace p essu e by he Pe se e ance o e in combina ion wi h o bi al images om he Ma s
Exp ess and Ma s Reconnaissance O bi e missions. The s udy s a s a L
s
∼13.3° in MY36 (6 Ma ch 2021) and
ex ends up o L
s
∼30.3° in MY37 (28 Feb ua y 2023). We ocus on he cha ac e iza ion o he majo
a mosphe ic phenomena a synop ic and plane a y‐scales. These a e he he mal ides (measu ed up o he six h
componen ), long‐pe iod p essu e oscilla ions (pe iods >1 sol), he Aphelion Cloud Bel , and he occasional
de elopmen o egional dus s o ms o e Jeze o. We p esen he seasonal e olu ion o he ampli udes and
phases o he he mal ides and hei ela ion wi h he a mosphe ic dus con en (op ical dep h). Th ee egional
dus s o ms and one pola s o m ex ending o e Jeze o p oduced an inc ease in he diu nal and semidiu nal
ampli udes bu esul ed in in e se esponses in hei phases. We show ha he p ima y egula wa e ac i i y is
due o ba oclinic dis u bances wi h pe iods o 2–4 sols and ampli udes ∼1–15 Pa inc easing wi h dus con en ,
in good ag eemen wi h heo e ical p edic ions by model calcula ions. The spacec a images show a numbe o
a c‐shaped, spi al and i egula cyclonic o ices, aced by dus and clouds a he edge o he No h Pola Cap,
ha could be behind some o he p essu e oscilla ions measu ed a Jeze o.
Plain Language Summa y We s udy a mosphe ic dis u bances obse ed as clouds and dus in
images ob ained om o bi ing spacec a , wi h simul aneous p essu e measu emen s on he su ace o Ma s by
he Pe se e ance o e on Jeze o c a e a la i ude 18° No h. The analysis ocuses on he no he n hemisphe e in
Ma ian Yea 36. We s udy he seasonal e olu ion o he ampli udes and phases o he he mal ides
(a mosphe ic oscilla ions in empe a u e and p essu e o ced by sola hea ing) and hei ela ion wi h he dus
con en o he a mosphe e and he p esence o clouds, including he di e en ypes o dus s o ms eaching he
c a e Jeze o. The images show a numbe o a c‐shaped, spi al, ing‐like and i egula o a ing o ices, aced
by dus and clouds a he edge o he No h Pola Cap ha could be behind some o he e ec s obse ed in
p essu e a Jeze o. We de ec wa e ac i i y wi h pe iods o 2–4 sols (a Ma ian day) and ampli udes ∼1–15 Pa
ha inc ease wi h he dus con en , in good ag eemen wi h heo e ical p edic ions by Gene al Ci cula ion
Models.
1. In oduc ion
Ma s has a ich and a ied me eo ology, s ongly in luenced by daily and seasonal insola ion cycles and whe e
apid changes de elop due o he low a mosphe ic mass and a sho adia i e ime cons an (Zu ek, 2017). Ob-
se a ions o Ma ian a mosphe ic phenomena ha e been ypically ca ied ou wi h elescopes on Ea h and in
nea ‐Ea h space, wi h spacec a o bi ing he plane , and wi h lande s and o e s on he su ace (James
e al., 2017). S udies o pa icula me eo ological phenomena a e usually pe o med ocusing on jus one o hese
da a se s. Bu , hey a ely ocus on bo h spacec a imaging and in si u obse a ions. In his wo k we use daily
images ob ained in he isible‐op ical ange wi h he Visual Moni o ing Came a (VMC) onboa d Ma s Exp ess
RESEARCH ARTICLE
10.1029/2024JE008565
Key Poin s:
•We s udy he su ace p essu e and he
he mal ides and wa es, om he i s
Ma ian Yea , ob ained by he o e
Pe se e ance a Jeze o
•We co ela e p essu e a iabili y and
oscilla ions wi h dus s o ms, clouds
and ba oclinic cyclones s udied om
images aken om o bi
•We p esen he ela ionships be ween
he su ace p essu e and ides up o six
componen s, wi h he op ical dep h
measu ed a Jeze o
Co espondence o:
A. Sánchez‐La ega,
[email p o ec ed]
Ci a ion:
Sánchez‐La ega, A., La sen, E., del Rio‐
Gaz elu u ia, T., He nández‐Be nal, J.,
O dóñez‐E xeba ía, I., Hueso, R., e al.
(2025). Ma ian a mosphe ic dis u bances
om o bi al images and su ace p essu e a
Jeze o C a e , Ma s, du ing Ma ian Yea
36. Jou nal o Geophysical Resea ch:
Plane s,130, e2024JE008565. h ps://doi.
o g/10.1029/2024JE008565
Recei ed 28 JUN 2024
Accep ed 19 DEC 2024
© 2025 The Au ho (s).
This is an open access a icle unde he
e ms o he C ea i e Commons
A ibu ion‐NonComme cial License,
which pe mi s use, dis ibu ion and
ep oduc ion in any medium, p o ided he
o iginal wo k is p ope ly ci ed and is no
used o comme cial pu poses.
SÁNCHEZ‐LAVEGA ET AL. 1 o 26
(MEX) (He nández‐Be nal e al., 2024b; Sánchez‐La ega e al., 2018a) and wi h he MARCI (Ma s Colo
Image ) ins umen onboa d Ma s Reconnaissance O bi e (MRO) (Bell III e al., 2009; Can o e al., 2010). We
combine hem wi h simul aneous in si u measu emen s om he Ma s En i onmen Dynamics Analyze (MEDA)
ins umen onboa d he o e Pe se e ance in ope a ion in Jeze o C a e since 18 Feb ua y 2021 wi h landing a
longi ude 77.45°E and la i ude 18.44°N (Rod íguez‐Man edi e al., 2021,2023).
This esea ch ocuses on synop ic (o mid‐scale) and plane a y‐scale phenomena as hey e ol e in empo al scales
app oxima ely ≥1 sol, speci ically on wa e dis u bances, dus s o ms and he mal ides (see Sánchez‐La ega
e al., 2024 o a classi ica ion o space and ime scales). P essu e has been shown o ha e high sensi i i y and
eliabili y as a e e ence magni ude o ack he mid‐ and la ge‐scale dynamical p ocesses in he a mosphe e (Hess
e al., 1977,1980; Ryan & Hen y, 1979; Wilson & Hamil on, 1996; Ha i e al., 2014,2024; Ban ield e al., 2020;
Ma inez e al., 2017; S eele e al., 2021; Rod íguez‐Man edi e al., 2023; Sánchez‐La ega e al., 2023 (pape 1);
Zu i a‐Zu i a e al., 2022; He nández‐Be nal e al., 2024a).
This s udy co e s one Ma ian Yea (see Can o e al., 2010 o he MY nume a ion), s a ing on Pe se e ance sol
16 (L
s
∼13.3° MY 36, 6 Ma ch 2021) and ex ending o sol 720 (L
s
∼30.3° MY 37, 28 Feb ua y 2023). Du ing
his pe iod, p essu e da a we e also acqui ed simul aneously by o he su ace missions loca ed in nea ly equa o ial
la i udes: he o e Cu iosi y (4.6°S, 137.4°E), he pla o m Insigh (4.5°N, 135.6°E) ha ope a ed un il 21
Decembe 2022, and he o e Zhu ong (25.07°N, 109.92°E) ha was ac i e be ween 27 June 2021 and 6 May
2022. The e o e, ou analysis o he a mosphe ic pe u ba ions de ec ed in he images ob ained om o bi can be
o in e es in u he compa a i e s udies o he p essu e measu emen s pe o med a hese o he loca ions.
This a icle is o ganized as ollows. In Sec ion 2, we p esen he da a sou ces used and he me hodology ollowed in
he analysis o he su ace p essu e and o bi al images. In Sec ion 3, we p esen he s udy o he p essu e mea-
su emen s in Jeze o wi h Sec ions 4and 5de o ed o he s udy o he mal ides and ba oclinic wa es, espec i ely.
In Sec ion 6, we p esen he di e en phenomena obse ed in he images o he no he n hemisphe e, o de ed by
sola longi ude pe iods in which each a mosphe ic phenomenon de elops. Finally, in Sec ion 7, we in e p e hese
obse a ions in he con ex o he mal ides, dus s o ms and ba oclinic cyclones and hei ela ion o he amoun o
a mosphe ic dus measu ed o e Jeze o. We conclude wi h a poin ‐by‐poin lis ing o he main esul s.
2. Da a Analysis
The me hodology and echniques employed in his a icle o he analysis o MEDA p essu e measu emen s ha e
been desc ibed in p e ious a icles (Rod íguez‐Man edi e al., 2023; Sánchez‐La ega e al., 2023, he eina e
called pape 1; Jaakonaho e al., 2023; Ha i e al., 2024). In pa icula , he me hod o calcula e he idal com-
ponen s and long pe iod wa es was desc ibed in Sánchez‐La ega e al. (2023), which co e ed hal o he pe iod
s udied in his a icle (up o sol 460, L
s
∼241°). Da a a e a ailable in Rod iguez‐Man edi and de la To e
Jua ez (2021).
Fo he su ey o a mosphe ic phenomena, we ha e used images aken by wo ypes o came as onboa d wo
spacec a wi h di e en and complemen a y o bi s. MEX is a spacec a in a pola o bi wi h a pe icen e a an
al i ude ∼300 km, an apocen e a an al i ude ∼10,000 km and an o bi al pe iod ∼7.5 h , allowing o obse e Ma s
wi h di e en phase angles and local imes (He nández‐Be nal e al., 2024b; Sánchez‐La ega e al., 2024). In
con as , MRO has a sun‐synch onized nea ly ci cula o bi , wi h an al i ude o e he su ace o ∼250–316 km and
a pe iod ∼1.86 h (Zu ek & Sm eka , 2007). MRO obse es he same a ea nea ly e e y 24 h a he same Local
Ma ian Time, a ound 14–15 h .
VMC is a ame came a o 640 ×480 pixels co e ing he spec al ange ∼400–650 nm wi h a Field o View
(FOV) o 40° ×30° (He nández‐Be nal e al., 2024b; O ms on e al., 2011; Sánchez‐La ega e al., 2018a). The
came a akes a sequence o images in each o bi al obse a ion block assigned o he came a wi h a spa ial es-
olu ion a nadi a ying be ween ∼300 m and 12 km, he la e allowing co e age o he en i e Ma ian disk. We
ha e analyzed VMC images (2024) using he Elkano so wa e desc ibed by He nández‐Be nal e al. (2021). We
also analyzed he op ical channel images o he MARCI came a, which has a wa eleng h co e age om 437 o
718 nm eaching a esolu ion o 1 km/pixel (Bell III e al., 2009; Can o e al., 2010). MARCI cap u es obse -
a ions o he en i e plane e e y sol by combining da a om 13 consecu i e o bi s (MARCI images, 2024). The
Local T ue Sola Times (LTST) a he cen e o he obse ed swa h ange a ound 15:00 ±02:00 h . We combined
MARCI ames (scans o e he en i e plane o iles) and p ojec ed hem in pola o ec angula maps in he
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Me eoma s so wa e (O dóñez‐E xebe ia e al., 2022). This so wa e allows na iga ion (longi ude and la i ude
g id and local ime) and measu emen o dis ances on he Ma ian su ace. Complemen a ily, we use he so wa e
ISIS‐USGS (2024) o he p ocessing and map p ojec ion o selec ed MARCI iles and QGIS (2024) o he
co esponding measu emen s.
Because o he no he n equa o ial la i ude o Pe se e ance a 18.5°N, we limi ou image su ey and analysis on
synop ic‐scale dis u bances e ol ing in he no he n hemisphe e, wi h he excep ion o hose phenomena ha
ex end o bo h hemisphe es, such as egional dus s o ms. A classi ica ion scheme o he s udied phenomena in
e ms o ei he hei empo al and spa ial scales, o hei loca ion on Ma s and seasonal dis ibu ion has been
p esen ed in Figu es 1–3 in Sánchez‐La ega e al. (2024). We ha e pe o med eloci y measu emen s o global
mo ions o wea he sys ems and local mo ions o clouds and dus masses wi hin hem, ollowing he iden i ica ion
and acking o well‐de ined ea u es ( hei cen e s o hei edges) on images sepa a ed by a known empo al
in e al. In VMC, he e is a wide a ie y o ime in e als be ween images used o acking. Typically, we obse e
blocks sepa a ed by 30 min, 2–3 h , and a whole day. In MARCI, he ime in e al be ween successi e swa hs
cap u ing he same egion depends on la i ude. Comple ing a pola o bi in abou 2 h , he spacec a can obse e
high‐la i ude a eas on e e y pass, p o iding highe empo al esolu ion. Nea he equa o , howe e , Ma s's
o a ion shi s he loca ion longi udinally, esul ing in in e als o o e 24 h be o e he same egion is e isi ed.
3. Su ace P essu e a Jeze o
In Figu e 1a we show he p essu e measu emen s along each sol o e he s udied pe iod and in Figu e 1b he
seasonal e olu ion (sol o sol) o he mean daily p essu e in Jeze o. The obse ed beha io o he p essu e ollows
Figu e 1. Su ace p essu e and op ical dep h measu ed a Jeze o. (a) Daily su ace p essu e ( e ical axis LTST, Local T ue Sola Time) as a unc ion o he sol numbe
measu ed by MEDA on boa d Pe se e ance. The p essu e is gi en in Pascal (Pa). Gaps in he measu emen s caused by limi ed esou ces o he mission and ope a ions
such as ock sampling appea in g ay. (b) Seasonal e olu ion o he daily mean p essu e be ween sols 16 and 716 (L
s
=13° in MY 36 o L
s
=30° in MY 37). Black do s
and g ays ba s ep esen he mean p essu e and i s s anda d de ia ion o each sol. The o ange do s a e p edic ions by he Ma s Clima e Da abase o he s anda d
clima ology and a e age sola condi ions. (c) Di e ences o maximum and minimum p essu es ela i e o hei mean alue o each sol; (d) The seasonal e olu ion o
he isible‐op ical dep h measu ed wi h Skycam (600–800 nm) and Mas cam‐Z (880 nm) on boa d Pe se e ance. The iden i ica ions co espond o he ollowing cases:
CL (clouds), DS‐1 (Dus S o m 1, i s egional s o m o e Jeze o), DS‐A (Dus S o m A), DS‐C (Dus S o m C), DS‐NPC (Dus S o m a he edge o he No h Pola
Cap passing close o Pe se e ance).
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he expec ed pa e n om he cycle o pola condensa ion and sublima ion o CO
2
and he in luence o he amoun
o dus suspended in he a mosphe e, measu ed as opaci y in Figu e 1d, changes he daily ange o p essu e da a
(Figu e 1c) simila ly o wha was obse ed by Viking (Ryan & Hen y, 1979). Lowe dus con en and highe cloud
abundance (no shown, e. g. Figu e 4 in Smi h e al., 2023) occu ed app oxima ely om L
s
∼0° o L
s
∼130°,
when sol‐ o‐sol a ia ions emained app oxima ely cons an . This pe iod was ollowed by an epoch o high a -
mosphe ic dus opaci y om L
s
∼130° o L
s
∼360° wi h la ge sol‐ o‐sol a ia ions (Figu e 1c). The a i al o
dus s o ms o e Jeze o du ing his second epoch is e ealed in he op ical opaci y measu emen s pe o med by
Pe se e ance (Figu e 1d). The op ical dep h was measu ed on a daily basis a di e en LMSTs om images
ob ained by he came as Mas cam‐Z and Skycam (Lemmon e al., 2022) and TIRS on MEDA (Smi h e al., 2023).
The i s egional s o m o e Jeze o occu ed a L
s
∼153–156° (sols 312–318) (labeled DS‐1 meaning dus s o m
1 in igu es in his pape ) and was analyzed in p e ious pape s (Lemmon e al., 2022; Mungui a e al., 2023;
Sánchez‐La ega e al., 2023). We ex end i s s udy in Sec ion 6.4. A no h pola s o m, no di ec ly a i ing a
Jeze o, is analyzed in Sec ion 6.5. The second and hi d s o ms di ec ly a ec ing Jeze o co esponded o he
egional e en s known as A (L
s
∼218°, sol 425 and labeled DS‐A in igu es in his pape ) and C (L
s
∼314°, sol
575 and labeled DS‐C in igu es in his pape ) (Kass e al., 2016; Ma in‐Rubio e al., 2024), and a e s udied in
Sec ions 6.6 and 6.7. A la e inc ease o opaci y co esponds o he close passage o a s o m e ol ing a he
no he n edge o he pola cap (L
s
∼358°, sol 656; labeled as DS‐NPC in igu es in his pape ) and is documen ed
in Sec ion 6.8.
4. Tide Ampli udes and Phases
Figu es 2a–2 show he seasonal e olu ion o he ampli ude o he six idal componen s (S
i
, i =1–6) co e-
sponding o pe iods o 24, 12, 8, 6, 4.8 and 4 h (see Pape 1 o de ails o he measu emen s and da a analysis). Fo
L
s
>130°, he co ela ion o he ampli udes o he diu nal (S
1
) and semidiu nal (S
2
) componen s wi h he op ical
dep h is e iden because bo h ollow he dus s o m e en s (Figu es 2a and 2b; see Sec ion 7.1). The ampli udes S
3
o S
6
ollow dual beha io . The odd componen s S
3
and S
5
show a simila pa e n wi h a peak ampli ude on sols
∼90–100 (L
s
∼50°) and a minimum a ound sol 200(L
s
∼100°) (Figu es 2c–2e). The e en componen s S
4
and S
6
exhibi ed nea ly simul aneous maximum ampli udes a sols ∼380 (L
s
∼191°) and ∼640 (L
s
∼350°) and a b oad
minimum om sol ∼80 o 260 (Figu es 2d–2 ). This dual beha io was also obse ed by Insigh o S
3
o S
6
(He nández‐Be nal e al., 2024a). As a compa ison, we show he calcula ions acco ding o he Ma s Clima e
Da abase (MCD 6.1) by he Labo a oi e de Mé éo ology Dynamique (LMD) (Fo ge e al., 1999) o s anda d
clima ology and a e age sola condi ions, and he p e‐landing p edic ions om he Ma s Wea he Resea ch and
Fo ecas ing (Ma sWRF) o he inne mos nes o Jeze o c a e (domain 5 wi h a ho izon al esolu ion o abou
1.5 km) (Newman e al., 2021). In gene al he Ma ian PCM esul s ep oduce he beha io o he idal ampli udes
easonably well. The e is some disag eemen in S
1
in he ange o sols 120–290 (L
s
=62°–141°) and o S
3
a ound
sols 40–160 (L
s
=25°–80°), bu in gene al he ag eemen is e y good, in pa icula o S
2
and S
4
‐S
6
, which
alida es he measu emen s. A de ailed s udy o he ela ionship be ween ides and wa e ice and dus op ical
dep h is p esen ed in Sec ion 7.1.
The seasonal beha io o he phases o he six idal componen s is mo e complex (Figu es 2g–2h). Componen s
S
1
‐S
3
showed a ying deg ees o a iabili y up o sol 290 (L
s
∼140°). The phase o he diu nal componen
showed a change o ∼11 h (∼½ cycle) be ween sols 130 and 210 (L
s
∼66°–102°), and hen had punc ual de-
c eases o 2–4 h du ing he s o ms excep o s o m DS‐C ha unde wen a comple e phase e e sal (24 h ). The
phase o he semidiu nal componen showed a la ge d op o 4 h wi h a minimum in sol 280 (L
s
∼136°) and hen
punc ual inc eases o ∼2 h du ing he ou s o ms. The phase o componen 4 is ela i ely cons an , while he
phase o componen 3 was noisie and showed a la ge a iabili y. The phases o ides 5 and 6 (no shown in
Figu e 2) we e signi ican ly noisie du ing ha pe iod and could be a ec ed by he measu emen s a egy o he
MEDA ins umen esul ing in many gaps in MEDA measu emen s (g ay egions in Figu e 1a; o a desc ip ion o
he MEDA measu emen s a egy see Rod íguez‐Man edi e al., 2023). In pa icula , he dus y pe iod was
abundan in ock sampling ac i i ies ha u he limi ed MEDA measu emen s wi h many sols wi h p essu e da a
acqui ed in blocks o 15 min sepa a ed by almos 1 hou .
5. Long‐Pe iod Wa es
We ha e s udied he long‐pe iod oscilla ions (>1 sol) ha occu a ound he daily mean p essu e end, using he
same me hodology as in pape 1, i. e. calcula ing he esiduals o polynomial i s o sol sec o s ha ypically co e
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>60 sols acco ding o he p essu e cycle shown in Figu e 1b. The esul ing de ended p essu e is shown in
Figu e 3a, whe e he la ge‐scale a mosphe ic phenomena a e labeled in he igu e. The esul s clea ly show he
exis ence o wo epochs. In he i s epoch, co esponding app oxima ely o he i s hal o he Ma ian yea wi h
less suspended dus (Figu e 1d), he peak o peak ampli udes o he long‐pe iod wa es a e low, on a e age 1.6 Pa
(sols 80–288, L
s
∼40°–140°). In he second epoch, co esponding o he dus y epoch (sols 288–720, L
s
∼140°–
30°), he ampli udes a e highe , on a e age ∼4.2 Pa, bu wi h peaks eaching up o 18 Pa. The mos p onounced
Figu e 2. Seasonal beha io o he ampli udes and phases o he idal componen s. (a)–(b) Diu nal and semidiu nal ampli udes S
1
and S
2
(black poin s), wi h clouds (CL)
and dus s o m e en s (DS) iden i ied as in Figu e 1. (c)–( ) Ampli ude o he componen s 3 o 6 (S
3
o S
6
) (black poin s). In panels (a)–( ) he MCD p edic ions a e
shown by he o ange line and in panels (a)–(d) he GCM‐Ma sWRF model p edic ions by a blue line. (g) Phase o he diu nal (black line) and semidiu nal (blue line)
componen s wi h ea u es iden i ied as in panel (a). (h) Phase o he e diu nal ( ed line) and qua e diu nal (g een line) componen s wi h ea u es iden i ied as in
panel (a).
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inc eases in ampli ude (up o ∼5–8 Pa la ge ) ook place du ing dus s o ms (DS‐1, DS‐A, DS‐C, DS‐NPC). We
also made a en a i e iden i ica ion o he impac o o he phenomena, such as he dus spi als ha de elop a
No h Pola Cap edge (p oducing ampli udes ∼2.5 Pa) and he Double Annula Cyclone DAC (∼1.2 Pa). The
de ails o he di e en cases s udied in he images a e p esen ed in he ollowing sec ions.
We ha e calcula ed he pe iod o hese oscilla ions as in pape 1 om he ime sepa a ion be ween consecu i e
peaks. The esul is shown in Figu e 3b. The dominan pe iod is be ween 2 and 4 sols, wi h a mean alue o
3.8 ±1.9 sol.
6. Imaging Synop ic and Plane a y‐Scale Dis u bances
In his sec ion, we classi y and s udy he di e en ypes o synop ic and plane a y‐scale a mosphe ic phenomena
isible in VMC/MEX and MARCI/MRO images, and look o hei possible ela ionship wi h he p essu e ob-
se a ions p e iously desc ibed. We ocus on dis u bances in he No he n Hemisphe e, bu we also conside
egional dus s o ms p opaga ing om he Sou h. Sánchez‐La ega e al. (2024) p esen a schema ic classi ica ion
o he main Ma ian a mosphe ic dis u bances. In he speci ic case o he Dus S o ms, an analysis o hei s a-
is ics, size and ae og aphical and empo al dis ibu ion du ing his same Ma ian yea (MY 36) can be ound in
Guha e al. (2024).
Figu e 3. Seasonal e olu ion o he long‐pe iod p essu e oscilla ions (>1 sol) a Jeze o o e one Ma ian Yea . (a) De ended p essu e wi h some o he phenomena
discussed in he ex iden i ied by hei ac onyms. Dus s o m spi als a he edge o he No h Pole Cap and he double annula cyclone (DAC) ook place along he sols
be ween magen a and g een ba s, espec i ely. The dus s o ms 1 (DS1), A (DS‐A), C (DS‐C) ook place along he sols be ween blue ba s. (b) Pe iod o he oscilla ions.
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6.1. No h Pole Edge Dus Cyclones (Ls =0°–90°)
In ense a mosphe ic ac i i y occu s a he edge o he No h Pola Cap du ing he sp ing season. Dus s o ms wi h
a a ie y o shapes (i egula , ex u ed, a cs and spi als) and sizes anging om ∼1,000 o 2,000 km o m and
disappea on sho empo al scales o 1–3 sols (Ba nes e al., 2017; Guzewich e al., 2015; Hea ens, 2017; Hinson
& Wang, 2010; Kah e e al., 2017; Mon abone e al., 2015; Sánchez‐La ega e al., 2018a,2022,2024) (Figu e 4).
They a e iden i ied as “S o ms NP edge” in he p essu e ampli ude oscilla ions (Figu e 3a). The e can appea up o
4–6 cyclones pe la i ude band (Figu e 4b), wi h some long a cs eaching leng hs o ∼4,000 km. In some cases
he e a e wa e ‐ice cloud ields a e associa ed wi h hese s o ms (Figu es 4c and 4d), indica ing ha he dis u -
bances ex end om he su ace (whe e hey li he dus ) o he middle a mosphe e whe e hey o m condensa ion
clouds. The mos in ense ac i i y akes place in he longi ude sec o 310°E–330°E and in la i udes 50°N–80°N,
ollowing he e ea o he No h Pola Cap (Figu e 5). These s o ms mo e p edominan ly eas wa d, some imes
wi h a no hwa d componen (di ec ion indica ed by a ows in Figu e 5). We ha e measu ed a e aged ansla ion
eloci ies <V>= +20 o +35 ms
−1
o he a c‐shaped ea u es (VMC/MEX images, sols 16–38, L
s
=14°–25°,
Figu e 4. Selec ed cyclone dus s o ms a he No h Pola Cap edge (L
s
=0°–45°) a e ma ked wi h black a ows in (a)–(b).
(a) 30 Ma ch 2021, sol =39, L
s
=24.5° (VMC/MEX). (b) Pola map showing a se ies o i e s o ms, 31 Ma ch 2021,
sol =40, Ls =24.9° (MARCI/MRO). (c) 31 Ma ch 2021, sol =40, Ls =24.9° (MARCI/MRO). This is he same s o m as in
(a), and he le mos in (b). (d) 17 May 2021, sol =86, Ls =46.4° (MARCI/MRO). The blue a ows in panels (c)–(d) show
he accompanying wa e ice clouds.
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Ma ch 2021) and <V≥3 o 16 ms
−1
o 10 spi al cyclones (MARCI/MRO images be ween sols 40 and 800
(L
s
=25°–43°, Ap il–May 2021). Taking in o accoun ha he ime in e als a e longe han one day and ha he
esolu ion o MARCI images is ∼1 km (nadi iew) and o VMC ∼5–10 km (a e age MEX dis ance o Ma s), he
e o s in he eloci y measu emen s a e e y low. Howe e , we es ima e ha in insic changes in he shape o he
ace s and in he cu so poin ing can gi e eloci y e o s o 1–2 ms
−1
. The sho es dis ance o Pe se e ance
eached by one o hese spi als was ∼2,600 km in sol 40 (L
s
∼25°, 31 Ma ch 2021).
6.2. Double‐Annula Cyclone (DAC) (L
s
=120°–140°)
The DAC is a seasonally ecu en dis u bance ha o ms a dawn in he longi ude ange ∼270°–330°E and a
subpola la i udes nea 60°N, dissipa ing du ing diu nal hou s, and eappea ing again he nex sol (Can o
e al., 2002,2010; Gie asch e al., 1979; Sánchez‐La ega e al., 2018b). I s o ici y is cyclonic wi h measu ed
angen ial eloci ies ∼5–20 ms
−1
(±1 ms
−1
) a 10 km al i ude. I appea s some imes as a single ing o wa e ‐ice
clouds (ma ked as “cen e ” in Figu e 6) and some imes wi h wo coupled cyclones (eas and wes ), each wi h a
size o 600–800 km (Sánchez‐La ega e al., 2018b). Du ing MY 36, i was obse ed om L
s
∼116°–134° (sols
239–276) (Figu e 6). The wes e n cyclone was placed a la i udes 60°N o 66°N and sligh ly no hwa d om he
eas e n cyclone a la i udes 58°N o 62°N, wi h bo h occupying a la ge zonal ex en in longi ude om ∼255°E o
345°E. Thei cen e s emained sepa a ed by abou 1,550 km. Bo h cyclones mo ed no heas wi h mean eloci ies
<V>= +0.5 o +3.7 m/s (de i ed om acking hei cen e s on MARCI images). The sho es dis ance o
Pe se e ance eached by he eas e n cyclone was ∼4,500 km in sol 278 (L
s
∼135°, 30 No embe 2021).
6.3. Aphelion Cloud Bel (L
s
=55°–140°)
The Aphelion Cloud Bel (ACB) de elops p og essi ely du ing he aphelion season, when dus con en is
minimum (Clancy e al., 2017; Wang & Inge soll, 2002; Wol e al., 2019). Wa e ‐ice clouds o m o e he
Figu e 5. (a) La i ude loca ion and displacemen o dus s o ms (a cs, spi als, i egula shape) a he edge o he No h Pola Cap o L
s
=0°–90° (do : cen e o he
ea u e). The same ea u e is iden i ied by a black line joining consecu i e do s. (b) Map showing he acks (black line joining do s) o he s o ms shown in panel (a). The
a ows ma k he mo ion di ec ion. The loca ion o Pe se e ance is indica ed by he blue‐ou lined whi e disk.
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olcanos and co e a g ea pa o he equa o ial band be ween la i udes ∼30°N and 20°S, wi h a la ge cloud
concen a ion om longi udes 220°E o 360°E (Figu e 7a).
Inspec ion o MARCI images du ing his pe iod shows he cen al pa o he Sy is Majo a ea co e ed wi h
wa e ‐ice clouds owa d L
s
∼100°, wi h a highe densi y o clouds eaching Jeze o mos ly on sols 284–305
(L
s
∼138°–149°) (Figu es 7b–7d), inc easing he op ical dep h o he a mosphe e (Lemmon e al., 2022;
Smi h e al., 2023). This is consis en wi h he high densi y cloud de ec ion om L
s
∼130°–150° by wo di e en
Pe se e ance ins umen s by Toledo e al. (2023) and Pa el e al. (2023).
The de elopmen o he ACB and he a i al o clouds a Jeze o a ec ed he diu nal and semidiu nal ides
(Figu es 2a, 2b, and 2g), which ollowed a complemen a y end. Hinson and Wilson (2004) ha e shown he
s ong coupling ha exis be ween he he mal ides and he adia i ely ac i e wa e ice clouds. Wi h he
beginning o he ACB pe iod, S
1
dec eased, becoming essen ially null in sols 117–131 (L
s
∼60°–67°) and in sols
189–199 (L
s
∼93°–97°). Then, wi h clouds p esen in Jeze o, S
1
has a maximum in sol 300 (L
s
∼146°) ollowed
by a minimum in sol 306 (L
s
∼149°), wi h a maximum‐ o‐minimum p essu e change o 7 Pa. This beha io o S
1
ollows he e olu ion o he cloud opaci y measu ed by Toledo e al. (2023) and Pa el e al. (2023) ha ound an
inc ease in cloud opaci y a ound L
s
∼120°–150°. The S
2
componen had wo deep minima eaching essen ially
ze o a he beginning o he ACB pe iod in sols 46–57 (L
s
∼28°–33°) and a i s end in sols 287–290 (L
s
∼139°–
141°), and was la ge han he diu nal componen du ing mos o he ACB pe iod.
The phase o he diu nal componen showed a deep and p olonged dec ease o abou 8 h (1/3 d o he daily cycle)
om sols 130–210 (L
s
∼66°–102°) and hen inc eased o a maximum in sols 235–286 (L
s
∼114°–139°). In
pa allel, he phase o he semidiu nal componen showed a d op o 4 h (1/3 d o he semidiu nal cycle o 12 h )
s a ing in sol 230 (L
s
∼112°) bu wi h a deep minimum in sol 286 (L
s
∼139°) jus be o e he a i al o DS‐1.
6.4. Regional Dus S o m O e Jeze o (L
s
=150°–156°)
The i s dus s o m o he season in Jeze o (DS‐1) ini ia ed on 1 Janua y 2022 (L
s
=150.7°, sol 308) close o he
edge o he sou h pola cap (la i udes 35°S o 45°S and 95°E o 135°E) (Figu e 8). The s o m expanded apidly
Figu e 6. The double annula cyclone (DAC). (a) and (b) Two iews o DAC on 12 No . 2021 (sol 260, Ls =126°) (MARCI). (c) DAC well de eloped on 29 Oc . 2021
(sol 247, Ls =119.6°) (MARCI). (d) DAC on 17 No . 2021 (sol 265, Ls =128.6°) (VMC). (e) Plo showing he longi ude loca ion o he wo DAC cyclones in ime
(Wes and Eas edges and Cen e ). ( ) Map showing he displacemen in longi ude and la i ude o he wo DAC componen s.
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571–574 (Figu e 14b). These changes in S
1
occu ed 3–4 sols be o e he op ical dep h eached i s maximum alue
a Pe se e ance in sol 574, ha is, while he dus was s ill p opaga ing om he wes owa d Jeze o (Sec ion 6.7,
Figu e 12). A simila beha io was epo ed a Gale c a e (Figu e 11 in Zu i a‐Zu i a e al., 2022) sugges ing ha
his is a obus dynamical coupling on a plane a y scale. The semidiu nal ampli ude unde wen a d op o ∼2 Pa in
S
2
in sol 568, ha is, 3 sols a e he onse o he s o m, when he dus was s ill a om Jeze o. This was ollowed
by a sha p inc ease in S
2
o abou 21 Pa, eaching he maximum in sol 576, while i s phase shi ed by 2–3 h
be ween sols 567 and 579. The changes in he phases o he diu nal and semidiu nal componen s occu ed
simul aneously (Figu e 14b), bu he maximum in S
1
occu ed abou 8 sols ea lie han ha o he S
2
(Figu e 14a).
The s o m also a ec ed he ampli ude and phase o he e diu nal componen S
3
, bu wi h small changes, close o
he de ec ion limi o he e ie al.
Figu e 14. Changes in he ampli ude and phase o he ides du ing he e olu ion o Dus S o m C. (a) Ampli ude o he
diu nal, semidiu nal and e diu nal componen s oge he wi h he op ical dep h e olu ion. (b) Same as panel (a) bu o he
idal phases.
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6.8. No h Pola Edge Dus Cyclones (L
s
=335°–360° and 0°–17°)
This is he s a o a new season o o ma ion o dus cyclones a he edge o he NPC, an ac i i y ha con inues up
o L
s
=90° (see Sec ion 6.1). The i s s o m o he season was obse ed on 11 No embe 2022 (sol 615,
L
s
=336.8°) cen e ed a abou 52°N and 162°E. Subsequen ly, new cyclonic s o ms we e egula ly obse ed a
he edge o he NPC (see ano he example in Gebha d e al., 2023). The mos in e es ing cases a e hose in which
he s o m comes close enough o Jeze o o in oduce dus in o he skies o e Pe se e ance o o dis u b he
p essu e measu emen s. One such case occu ed be ween 18 and 27 Decembe 2022 (sols 650–659, L
s
=356°–
0.7°) (Figu e 15). A s o m ha we called DS‐NPC g ew up no h o Pe se e ance, e ol ing om a compac
ex u ed ea u e o an a c‐shaped s o m. The dis u bance mo ed eas wa d a 15 ms
−1
and i s cen e was
∼1,480 km no h o Pe se e ance on sols 654–655 (Figu es 15b and 15c). The edge o his s o m was only 585 km
Figu e 15. A compac dus s o m (a ow) e ol ing o an a c‐shape ea u e app oaching Pe se e ance on MARCI images.
(a) 21 Decembe 2022 (Ls =357.7, sol 653); (b) 22 Decembe 2022 (Ls =358.2, sol 654); (c) 23 Decembe 2022
(Ls =358.7, sol 655); (d) 27 Decembe 2022 (Ls =360.7, sol 659). In all hese images LTST ∼14 h . The blue‐ou lined whi e
disk ma ks he loca ion o Pe se e ance.
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om Pe se e ance, close enough o injec dus o e he o e . On sols 657–658 he op ical dep h da a show a peak
in opaci y (Figu e 1d) and he diu nal and semidiu nal ampli udes o he he mal ides aised hei p essu e
by ∼9 Pa (sol 659, L
s
=0.4° in MY37) and by ∼2 Pa (sol 655, L
s
=358.4° in MY36) (Figu es 2a and 2b),
espec i ely. Al hough smalle in ampli ude, his beha io emembe s wha was seen wi h majo s o ms. How-
e e , hei phases do no show a change in sols 650–660. The e is a p e ious peak in opaci y in sols 600–640, wi h
a co esponding inc ease in he ampli ude o he diu nal componen , his ime lea ing no clea signal in he
semidiu nal ide o in he phases. We did de ec a idal phase end simila o p e ious s o ms in sol 703 (L
s
∼22°),
wi h he diu nal phase d opping ∼2 h (∼1/12 h diu nal cycle) and semidiu nal inc easing by 3 h (∼1/8 h diu nal
cycle) simul aneously (Figu es 2a and 2b, 2b, and 2g). We hink hese phase changes a e no ela ed o s o m DS‐
NPC because he ime di e ence is a ound 40 sols. La e on, o he s o ms o med egula ly a he NPC and we e
obse ed up o he end o ou imaging su ey on 31 Janua y 2023 (L
s
=17.4° in MY37, sol 693). I should be
no ed ha hese dus s o ms a e also accompanied by clouds, p obably o med along wi h he s o m bu a highe
al i udes han whe e he dus is injec ed (see Sec ion 6.1, Figu e 4).
7. Discussion
In his sec ion, we s udy he e ec s and co ela ions be ween he synop ic and plane a y‐scale dis u bances
p esen ed in Sec ion 6and he long‐pe iod wa es and ides as cha ac e ized om he su ace p essu e mea-
su emen s by Pe se e ance p esen ed in sec ions 3‐5.
7.1. Dus and Cloud Op ical Dep h and Thei E ec s on Tides
We i s examine he ela ionship be ween he ampli udes o he he mal ides and he ae osol con en in he
a mosphe e as measu ed a Jeze o. Figu e 16a shows he compa ison be ween he no malized ampli udes o he
diu nal and semidiu nal componen s (i.e., he ide ampli ude di ided by he mean p essu e in ha sol) wi h he
ae osol op ical dep h acco ding o he empi ical o mula ion p oposed by Wilson e al. (2008) (and pape 1). The
co ela ion be ween he seasonal a ia ion o S
1
and S
2
wi h a linea unc ion on τ is good o L
s
∼130°–360°, ha
is, du ing he dus y pe iod. Howe e , no co ela ion is ound in he ange L
s
∼0°–130° when S
1
and S
2
show
opposed seasonal ends du ing he low‐dus pe iod, when he con ibu ion o he op ical dep h o he wa e ‐ice
clouds was signi ican (Pa el e al., 2023; Smi h e al., 2023; Toledo e al., 2023), and he o al τ ∼cons an
(Figu e 1d).
The ela ionship be ween he seasonal a ia ion o he combined idal ampli udes and he o al op ical dep h
measu ed a Jeze o is u he explo ed in Figu e 16b. He e, as in pape 1, we show ha he obse ed pa e n in he
seasonal e olu ion o he op ical dep h is simila o ha ollowed by a combina ion o a 50% o S
1
and S
2
componen s. This co ela ion sligh ly imp o es when he combina ion includes a mix u e o S
1
o S
4
ampli udes in
he ollowing pe cen ages: S
1
(27%), S
2
(53%), S
3
(16%) and S
4
(4%).
7.2. Long‐Pe iod Wa es
We ha e seen in Sec ions 6.1, 6.2, and 6.8 ha abundan cyclones de elop a he NPC edge du ing he L
s
pe iods
335°–360° and ∼0°–140° (app oxima ely he epoch o he ACB de elopmen ). They e ol e in he la i ude band
om ∼55°N o 75°N and ollow he pola ice‐cap e ea (Figu e 5). Mos o hese cyclones gene a e s ong
su ace winds ha li he dus up o 6–11 km (Sánchez‐La ega e al., 2022). O he cyclones, such as he ecu en
DAC (L
s
∼120°–140°), do no li dus bu o m clouds a heigh s ∼10–20 km (Sánchez‐La ega e al., 2018b). I
he obse ed p essu e oscilla ions a Jeze o, wi h ampli udes be ween 2 and 4 Pa and pe iods be ween 3 and 4 sols
(Figu e 3), a e ela ed o his cyclone ac i i y, he adius o ac ion o he low p essu e dis u bance associa ed wi h
he cyclonic o ici y would be la ge (by a ac o 2–3) han he o ex size as aced by dus and clouds. F om
he measu ed size o he obse ed cyclones L ∼1,000–2,500 km we ge wa enumbe s n∼(πRMcos 600)/
L∼2−5 (assuming he cyclone size is hal a wa eleng h) whe e R
M
is he adius o Ma s. I we use he adius
o ac ion o he dep ession (indica ed abo e) ins ead, hen n∼1–3 which is in ag eemen wi h p e ious wo ks
(Ba nes e al., 2017; Collins e al., 1996; Hinson & Wilson, 2021). Wa es wi h pe iods in he ange 2–5 sols (and
wa enumbe s 1–3) we e also in e ed om he signal lag in he p essu e da a measu ed a he same season a
Jeze o and a Gale c a e by Cu iosi y (Ba alio e al., 2022).
The ampli ude o he p essu e oscilla ions inc eased d ama ically a ound sol ∼300 (L
s
∼146°) wi h he s a o he
dus y season, and pa icula ly du ing he e olu ion o dus s o ms o e Jeze o, when peak o peak ampli ude was
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abo e 10 Pa (Figu e 3). The la ges ampli ude was ∼22 Pa, and i was measu ed du ing he dus s o m C on sols
∼560 o 580 (L
s
=307°–312°) jus be o e he dus eached i s maximum op ical dep h a Jeze o (Figu es 1d
and 14a).
Ba alio and Wang (2020) s udied he e olu ion o eddy ac i i y du ing la ge‐scale dus s o ms. He e, we ha e
analyzed he beha io o he p essu e oscilla ions along he Ma ian Yea 36 a Pe se e ance loca ion by con-
duc ing simula ions wi h he LMD Ma ian PCM (Plane a y Clima e Model) (Fo ge e al., 1999) ollowing he
me hod desc ibed in Lewis e al. (1999) and Millou e al. (2022). Figu e 17 shows p essu e oscilla ions as
ob ained om he simula ion in he egion o Jeze o c a e when il e ing he p essu e da a om he diu nal mean
and seasonal end. The simula ion desc ibed in his sec ion was ca ied ou wi h a 64 ×48 la /lon g id
Figu e 16. Rela ionships be ween he ampli udes o he he mal ides and he ae osol op ical dep h. (a) No malized
ampli udes o he diu nal S
1
and semidiu nal S
2
and hei ela ion wi h a linea unc ion o he op ical dep h gi en by
1.6τ+0.3. (b) Rela ionship be ween he op ical dep h and wo combina ions o he ampli udes o he ides.
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(2.8° ×7.5°, la i ude x longi ude), and 36 e ical le els, wi h a e ical esolu ion dec easing om 5 m nea he
su ace o 10 km a he model op (∼80 km). The physical ime‐s ep is ∼7 min and we use windows o 10° in L
S
(in
s eps o 0.5°). The e e ence simula ion is pe o med wi h wo‐momen ae osol sizes dis ibu ions o wa e ice
and dus . Dus pa icles a e ep esen ed by a logno mal pa icle size dis ibu ion wi h an e ec i e a iance o 0.5
and an e ec i e pa icle adius o 3 μm. This choice is d i en by be e ag eemen be ween simula ed and
obse ed opaci ies. The simula ion has been ca ied ou o e mul iple annual cycles o MY36 using he a ailable
MCS‐ and EMIRS‐de i ed column opaci y maps o ha yea (Mon abone e al., 2023), as a cons ain o he
simula ion o ma ch. In p ac ice, dus is injec ed om he su ace in o he PBL when he simula ed dus column
opaci y is lowe han ha in he column opaci y map so ha he ae osol and empe a u e dis ibu ions could each
a seasonally equilib a ed s a e. We use adia i ely ac i e dus , wa e apo and wa e ice clouds. The pe iod o he
Figu e 17. P essu e oscilla ions ob ained om a PCM simula ion in MY36 in he egion o Jeze o c a e , calcula ed as
esiduals be ween he simula ed mean daily p essu e and he mean p essu e o e a 10‐sols sliding window (seasonal end).
Uppe plo shows he ampli ude and he lowe plo shows he pe iod. The esul ing oscilla ions a e mos ly due o he
ba oclinic ac i i y.
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model simula ed oscilla ions ange om ∼2 sols (sol ange ∼380–470, Ls =190°–248°) o ∼8–20 sols (sol ange
180–290, Ls =89°–141°).
O e all, he model ep oduces he main end obse ed wi h MEDA (Figu e 3), wi h low ampli ude oscilla ions
ob ained du ing he i s hal (“clea season”) o he Ma ian yea and la ge ampli ude oscilla ions ob ained
du ing he second hal (“dus y season”). The seasonal end in he peak‐ o‐peak pe iods and ampli udes p edic ed
by he model ag ees well wi h ha obse ed o he ange o sols ∼10–150 (wi h pe iods 4–5 ±1.5sols) and
∼340–700 (wi h pe iods 3–4 ±1 sols). As obse ed, he a mosphe ic wa es ha e la ge ampli udes du ing he
dus y season. I could be emp ing o assign he oscilla ions obse ed du ing he pe iod om L
s
∼337° (sol 615) o
L
s
∼44° (sol 80, MY36) o he ansien dus cyclone ac i i y a he NPC edge (Figu es 4, 5 and 14). The model
and obse a ions a e consis en in his pe iod wi hin he global end, al hough he model p edic s highe am-
pli udes han obse ed (Figu es 3and 17). Cla i ica ion o his poin would equi e new simula ions, which is
beyond he scope o his pape .
Ba oclinic ins abili y induces wa es wi h pe iods <8 sols as obse ed by senso s on lande s (Ban ield e al., 2020;
Ba nes, 1980,1981,1984; Ba nes e al., 1993; Habe le e al., 2018; Zu i a‐Zu i a e al., 2022). The obse a ions
and measu ed p ope ies o cyclones om o bi (Ban ield e al., 2004; Ba alio e al., 2022; G eybush e al., 2019)
a e compa ible wi h hei ba oclinic o igin (Ba nes, 1984; Ba alio & Wang, 2020; Hinson & Wilson, 2021;
Hollingswo h & Kah e, 2014; Hun & James, 1979; Sánchez‐La ega e al., 2018b,2022). He e, we use he
maximum g ow h a e o ba oclinic dis u bances in Ma s' no he n hemisphe e o assess he de elopmen o he
obse ed cyclones a he No h Pola Cap edge. A use ul es ima e o he g ow h a e is gi en by he ba oclinic
index, de ined as (Ba alio e al., 2016; James & G ay, 1986; Lembo e al., 2017; Lindzen & Fa ell, 1980):
σBI =0.31
N



∂U
∂z



(1)
he e =2Ω sin φis he Co iolis pa ame e wi h φ he la i ude and Ω =7.08 ×10
−5
s
−1
he angula o a ion
eloci y o Ma s, N2(z) = g
T(z)[dT
dz (z) + g
Cp]is he B un ‐Väisäla equency whe e we used o he adiaba ic
g adien g/C
p
=4.5 K km
−1
, and ∂U
∂zis he e ical shea o he zonal wind eloci y (U). Al hough Equa ion 1was
de i ed o a cons an e ical wind shea , Lindzen and Fa ell (1980) a gue i s mo e gene al alidi y. We p ese e
in Equa ion 1 he coe icien 0.31 o ge he app oxima e ime‐scales in ol ed in he g ow h a e o he ba oclinic
dis u bances in Ma s. To calcula e he ba oclinic index σ
BI
, we use he MCD o s anda d clima ology and a e age
sola condi ions o ge he empe a u e and zonal wind maps (la i ude‐al i ude), T(z,φ) and U(z,φ), a he
Pe se e ance longi ude and o LTST anging om 7 o 12 h . We selec ed he alues o L
s
o ep esen a i e
cases o he obse ed wa e ac i i y. We hen calcula e he mean N(z) and (dU/dz) (z) in he la i ude ange ∼55°N–
65°N whe e he peak eloci y o he no he n eas wa d je s eam is p edic ed.
Figu e 18 shows he e ical p o iles o he g owing ime o he ins abili y ( he in e se o he ba oclinic index σ
BI
)
o he selec ed L
s
pe iods a 10:00 LTST. Globally, we can di ide he beha io o he g owing ime p o iles in o
wo pe iods. In he i s pa o he yea , o L
s
∼45°–135°, he as es g owing ime occu s a wo heigh s ∼4 and
22 km. Close o he su ace, he empe a u e p o ile in he model is con ec i ely uns able e en a 07:00 LTST in
he mo ning. The obse a ion o he dus spi als and simila ea u es in his epoch (Figu es 4, 5 and 15) sugges s
ha he ba oclinic ins abili y ac ually ex ends nea he su ace whe e he dus cyclones o m and he o ex winds
aise he dus (Hollingswo h & Kah e, 2014; Mulholland e al., 2016). Du ing he dus y pe iod (L
s
∼180°–360°),
he ampli ude o he su ace p essu e oscilla ions measu ed by Pe se e ance inc eases as does he amoun o dus
in he a mosphe e (Figu es 3and 17). The g owing ime o ba oclinic wa es in his pe iod has i s as es alues
e y close o he su ace a LTST 7–12 h and is qui e cons an wi h al i ude abo e 4 km. This ime o he yea
co esponds o he pola nigh in he no he n hemisphe e and o he de elopmen o he No h Pola Hood.
8. Summa y
We ha e used he Ma ian yea 36 as a case s udy o he ela ionship be ween su ace p essu e measu emen s and
he de elopmen o medium and la ge scale a mosphe ic phenomena in he no he n hemisphe e o Ma s obse ed
in o bi al images. Ou mos ele an indings a e
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•The mal ides: In he dus y pe iod (b oadly, L
s
∼130°–360°), he am-
pli udes o he diu nal and semidiu nal componen s o he daily p essu e
cycle co ela e wi h he op ical dep h measu ed a Jeze o and wi h he
de elopmen o dus s o m e en s nea Jeze o. No co ela ion is ound
om L
s
∼0°–130°, coinciding wi h he de elopmen o he ACB. The
ampli udes o he idal componen s 3 and 5 on he one hand, and 4 and 6 on
he o he , ollow a simila beha io . The seasonal e olu ion o he ae osol
op ical dep h co ela es well wi h a combina ion o 50% o he ampli udes
o he diu nal and semidiu nal componen s. The co ela ion imp o es
when combining he ampli udes o he ou componen s wi h a ious
empi ical weigh s domina ed as be o e by he con ibu ion o he semi-
diu nal and diu nal ides. The inc ease in op ical dep h p oduced by wa e
ice clouds co ela es well wi h an inc ease in he ampli ude o he diu nal
componen and wi h a p onounced d op in he semidiu nal componen .
•Dus Cyclones. Spi al, i egula and comma‐a c o ices aced by dus
we e obse ed a he edge o he No h Pola Cap (50°N–80°N) in he L
s
anges ∼0°–90°, 160°–190°, 335°–360° (MY 36) and 0°–17° (MY 37).
Thei ypical size is L ∼1,000–2,000 km and he mos ac i e a ea whe e
hey g ow is he Acidalia Plani ia (longi ude ∼330°E). These o ices
e ol e a dis ances om Pe se e ance ∼1,500 km (closes ) o 4,500 km
(on a e age). They a e mos p obably behind he p essu e oscilla ions
de ec ed a Pe se e ance wi h ampli udes o ∼1.5–4 Pa (ampli udes
inc easing wi h dus con en in he a mosphe e) and pe iods 2–4 sols. One
o hem (DS‐NPC a L
s
∼357°–360°) eached Pe se e ance, lea ing i s
imp in in he diu nal and semidiu nal ides. Thei p ope ies ag ee wi h a ba oclinic o igin and hei am-
pli udes and pe iods ag ee wi h he Ma ian PCM p edic ions.
•Double Annula Cyclone (DAC). The ecu en DAC, aced by wa e ice pa icles, was obse ed om
L
s
∼120°–140° a subpola la i udes nea 60°N. This peculia dis u bance, o ba oclinic o igin, g ows and
dissipa es wi hin each sol, while i ansla es slowly eas wa d, e ol ing a la ge dis ances om Pe se e ance
(4,500 km o 7,000 km along a la i ude ci cle). The p essu e oscilla ions de ec ed by Pe se e ance in his
pe iod p esen a small ampli ude (<2 Pa) and i is unce ain whe he he DAC con ibu es o hem.
•Aphelion Cloud Bel . The de elopmen o he ACB and he cloud a i al a Jeze o possibly a ec ed he diu nal
and semidiu nal ides. The diu nal componen was null a L
s
∼60°–67° and in L
s
∼93°–97° bu eached a
maximum a L
s
∼146° when clouds we e o e Jeze o, a end consis en wi h measu emen s o he wa e ‐ice
cloud op ical dep h. The phase o he diu nal componen unde wen a signi ican dec ease o abou 8 h (1/3 d
o he daily cycle) om L
s
∼66°–102° and hen a maximum a L
s
∼114°–139°. The ampli ude o he
semidiu nal componen was ze o a he beginning o he ACB a L
s
∼28°–33° and a i s end a L
s
∼139°–141°,
and has a maximum in be ween. In pa allel, he phase showed a d op o 4 h (1/6 h o he daily cycle) s a ing a
L
s
∼112° and wi h a p onounced minimum a L
s
∼139° when clouds a i ed a Jeze o. Compa a i ely, he
beha io o he diu nal and semidiu nal componen s, bo h in ampli ude and phase, ollowed a complemen a y
end.
•Dus S o ms on Jeze o. Fou episodes injec ed dus a he loca ion o Pe se e ance. (a) The i s egional s o m
(DS‐1) ook place om L
s
∼150°–156°. Expansion eloci ies we e o a ound 20‐25 ms
−1
, eaching an a ea o
4.1–8.7 ×10
6
km
2
. (b) The ecu en e en A (DS‐A) ook place be ween L
s
∼205°–235°. (c) The ecu en
s o m C (DS‐C) ook place be ween L
s
∼308°–318° showing a complex expansion beha io wi h eloci ies
be ween 16 and 26 ms
−1
(±1‐2 ms
−1
), eaching a egional scale wi h an a ea ∼2.9 ×10
7
km
2
. The dus al i ude
was ∼30 km a he la i ude o Pe se e ance, bu in he sou h i eached 60–80 km. (d) The ou h was a spi al
s o m (DS‐NPC) ha e ol ed a he edge o he No h Pola Cap a L
s
∼1 (MY37).
•Dus S o ms and ides. The ou dus s o ms p oduced i s a dec ease and hen a apid inc ease in he
ampli ude o he diu nal and semidiu nal ides (by a ac o ∼2, o ∼10–20 Pa). The phase o he diu nal
componen showed punc ual dec eases du ing he s o ms (∼2–3 h , 1/12 h‐1/8 h o he daily cycle) excep o
he case o DS‐C ha p oduced a ull phase change o 24 h . The phase o he semidiu nal componen showed
punc ual inc eases du ing he ou s o ms o ∼3 h (1/8 h o he daily cycle). In some cases, lags o 1–3 sols
Figu e 18. Ve ical p o iles o he g owing imes o ba oclinic dis u bances
associa ed wi h he no he n eas wa d je s eam cen e ed a la i ude ∼60°N
a he longi ude o he Pe se e ance o e (77.5°E) and a LTST =10 h o
selec ed alues o he sola longi ude L
s
(based on MCD da a).
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occu be ween he maximum in he op ical hickness and he maximum change in he idal ampli udes and
phases.
Fu u e wo k will aim o in e p e he phenomena desc ibed he e and hei e ec on su ace p essu e measu emen s
by means o nume ical models. Among o he phenomena, we need o unde s and he ela ionship be ween he
e ical and ho izon al dis ibu ion o suspended dus and wa e ‐ice clouds, he dus s o m p ope ies, and he
ampli udes and phases in he su ace p essu e associa ed wi h he componen s o he he mal ides. Ano he u u e
s udy is he de elopmen o models o he ba oclinic cyclones gene a ed a he edge o he NPC (such as he dus
spi als and he DAC and o he simila o ices) and he s uc u e o hei p essu e ield a la ge dis ances.
Da a A ailabili y S a emen
The images om he VMC/MEX and MARCI/MRO came as can be e ie ed om he e e ences MARCI
images (2024) and VMC images (2024). The MEDA/Pe se e ance p essu e measu emen s a e a ailable h ough
Rod iguez‐Man edi and de la To e Jua ez (2021). The so wa e is a ailable h ough he e e ences ISIS‐
USGS (2024) and QGIS (2024). The Ma s Clima e Da abase (MCD) om LMD can be accessed a h ps://www‐
ma s.lmd.jussieu. /ma s/access.h ml.
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Acknowledgmen s
This wo k has been suppo ed by G an
PID2019‐109467GB‐I00 unded by
MCIN/AEI/10.13039/501100011033/and
by G an PID2023‐149055NB‐C31 unded
by MICIU/AEI/10.13039/501100011033
and FEDER, UE, and by G upos de
In es igacion del Gobie no Vasco IT‐
1366‐19. Pa s o his wo k we e also
unded by he Aula EspaZio Gela, which is
suppo ed by a g an om he Dipu ación
Fo al de Bizkaia (BFA). EL and JHB we e
suppo ed by ESA Con ac No.
4000118461/16/ES/JD, Scien i ic Suppo
o Ma s Exp ess Visual Moni o ing
Came a and h ough he Facul y o he
Eu opean Space As onomy Cen e
(ESAC) ‐ Funding e e ence ESAC‐531.
The au ho s a e e y g a e ul o he en i e
Ma s 2020 science ope a ion eam.
Jou nal o Geophysical Resea ch: Plane s
10.1029/2024JE008565
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