116:
are all believed to have been dominated by lid tectonics for their entire history. In the mantle of both
Mercury and the Moon, heat is mainly lost by conduction across the lid, leading to low heat flows. Solomatov and Moresi used the term "stagnant lid" when they characterized the tectonic style that
264:
Stern, R.J., 2008. Modern-style plate tectonics began in
Neoproterozoic time: an alternative interpretation of Earth's tectonic history. In: Condie, K.C., Pease, V. (Eds.), When Did Plate Tectonics Begin on Planet Earth?. Geological Society of America Special Paper 440, pp.
117:
was present on Venus in 1996. They stated that Venus had plumes similar to Earth, that would rise to the surface, and cold "drips" of lithosphere would sink back down. Mars is also believed to have stagnant lid tectonics, albeit, much slower in comparison to Venus.
67:
is high enough where the lid cannot brittlely fail. This relationship relies heavily on the ratio of lithospheric strength to natural convective stresses. Hence, if lithospheric strength is greater than convective stresses, then there are stagnant lid tectonics.
83:
The lid will not participate in the underlying convection of the mantle. At the base of the lithosphere, where the lid is in contact with less viscous material, melts will form at the thermal boundary layer and cause drips, believed to be of
46:
minerals. The relative stability and immobility of the strong cooler lids leads to stagnant lid tectonics, which has greatly reduced amounts of horizontal tectonics compared with plate tectonics (which can also be described as
294:
Louro LourenƧo, D., Rozel, A. B., Ballmer, M. D., Gerya, T., & Tackley, P. J. (2018, April). Plutonic-squishy lid: a new global tectonic regime generated by intrusive magmatism on Earth-like planets. In
237:
Solomatov, V.S., Moresi, L., 2000. Scaling of time-dependent stagnant lid convection: application to small-scale convection on Earth and other terrestrial planets. J. Geophys. Res. 105, 21795ā21818
210:
Ogawa, M., Schubert, G., Zebib, A., 1991. Numerical simulations of three-dimensional thermal convection in a fluid with strongly temperature-dependent viscosity. J. Fluid Mech. 233, 299ā328.
228:
Solomatov, V.S., Moresi, L., 1997. Three regimes of mantle convection with non-Newtonian viscosity and stagnant lid convection on the terrestrial planets. Geophys. Res. Lett. 24, 1907ā1910.
277:
Stern, R. J. (2005). Evidence from ophiolites, blueschists, and ultrahigh-pressure metamorphic terranes that the modern episode of subduction tectonics began in
Neoproterozoic time.
255:
O'Neill, C., Jellinek, A.M., Lenardic, A., 2007a. Conditions for the onset of plate tectonics on terrestrial planets and moons. Earth Planet. Sci. Lett. 261, 20ā32.
328:
Breuer, D., & Spohn, T. (2003). Early plate tectonics versus singleāplate tectonics on Mars: Evidence from magnetic field history and crust evolution.
219:
Moresi, L., Solomatov, V.S., 1995. Numerical investigation of 2D convection with extremely large viscosity variations. Phys. Fluids 7, 2154ā2162.
55:
was recognised as a possible stable regime for convection on Earth, in contrast to the well-attested mobile plate tectonics of the current eon.
63:
A lid tectonic regime arises when the cold upper lithosphere is too viscous to participate in the underlying flow of the mantle. The lid's
76:
Many characteristics of a planetary body influence the presence and degree of lid tectonics. The temperature of a body's
80:, and the presence of water, strongly affect the rheological, composition, and thermal diagnostics of lid tectonics.
357:
77:
38:, and possibly existed on Earth during the very early part of its history. The lid is the equivalent of the
168:
352:
191:
183:
169:"A reassessment of the heat transport by variable viscosity convection with plates and lids"
147:
101:
52:
64:
346:
97:
35:
311:
Solomatov, V. S., & Moresi, L. N. (1996). Stagnant lid convection on Venus.
39:
152:
135:
85:
187:
113:
31:
196:
96:
Stagnant lid regime is the most common tectonic style that exists in the
88:
composition. This stagnant lid regime will not effectively mix a mantle.
43:
34:
that is believed to exist on several silicate planets and moons in the
109:
105:
51:). The presence of a stagnant lid above a convecting
8:
297:EGU General Assembly Conference Abstracts
195:
151:
330:Journal of Geophysical Research: Planets
313:Journal of Geophysical Research: Planets
126:
307:
305:
72:Factors contributing to lid tectonics
7:
273:
271:
251:
249:
247:
245:
243:
134:O'Neil C.; Roberts N.M.W. (2018).
14:
1:
176:Geophysical Research Letters
16:Aspect of planetary geology
374:
153:10.1016/j.gsf.2017.10.004
136:"Lid tectonics ā Preface"
188:10.1029/GL016i002p00179
22:commonly thought of as
92:Other planetary bodies
24:stagnant lid tectonics
140:Geoscience Frontiers
78:coreāmantle boundary
49:mobile lid tectonics
28:single lid tectonics
299:(Vol. 20, p. 491).
167:Gurnis M. (1989).
42:, formed of solid
358:Planetary geology
30:, is the type of
365:
337:
326:
320:
319:(E2), 4737-4753.
309:
300:
292:
286:
275:
266:
262:
256:
253:
238:
235:
229:
226:
220:
217:
211:
208:
202:
201:
199:
173:
164:
158:
157:
155:
131:
373:
372:
368:
367:
366:
364:
363:
362:
343:
342:
341:
340:
327:
323:
310:
303:
293:
289:
276:
269:
263:
259:
254:
241:
236:
232:
227:
223:
218:
214:
209:
205:
171:
166:
165:
161:
133:
132:
128:
123:
94:
74:
61:
17:
12:
11:
5:
371:
369:
361:
360:
355:
345:
344:
339:
338:
321:
301:
287:
267:
257:
239:
230:
221:
212:
203:
182:(2): 179ā182.
159:
125:
124:
122:
119:
93:
90:
73:
70:
65:yield strength
60:
57:
20:Lid tectonics,
15:
13:
10:
9:
6:
4:
3:
2:
370:
359:
356:
354:
351:
350:
348:
335:
331:
325:
322:
318:
314:
308:
306:
302:
298:
291:
288:
285:(7), 557-560.
284:
280:
274:
272:
268:
261:
258:
252:
250:
248:
246:
244:
240:
234:
231:
225:
222:
216:
213:
207:
204:
198:
197:2027.42/95533
193:
189:
185:
181:
177:
170:
163:
160:
154:
149:
145:
141:
137:
130:
127:
120:
118:
115:
111:
107:
103:
99:
91:
89:
87:
81:
79:
71:
69:
66:
58:
56:
54:
50:
45:
41:
37:
33:
29:
25:
21:
333:
329:
324:
316:
312:
296:
290:
282:
278:
260:
233:
224:
215:
206:
179:
175:
162:
143:
139:
129:
98:Solar System
95:
82:
75:
62:
48:
36:Solar System
27:
23:
19:
18:
40:lithosphere
347:Categories
146:(1): 1ā2.
121:References
86:peridotite
353:Tectonics
59:Formation
32:tectonics
265:265ā280.
44:silicate
279:Geology
102:Mercury
112:, and
104:, the
53:mantle
336:(E7).
172:(PDF)
110:Venus
106:Moon
334:108
317:101
192:hdl
184:doi
148:doi
26:or
349::
332:,
315:,
304:^
283:33
281:,
270:^
242:^
190:.
180:16
178:.
174:.
142:.
138:.
114:Io
108:,
100:.
200:.
194::
186::
156:.
150::
144:9
Text is available under the Creative Commons Attribution-ShareAlike License. Additional terms may apply.