Low-degree structure in Mercury's planetary magnetic field
The structure of Mercury's internal magnetic field has been determined from analysis of orbital Magnetometer measurements by the MESSENGER spacecraft. We identified the magnetic equator on 531 low-altitude and 120 high-altitude equator crossings from the zero in the radial cylindrical magnetic...
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| Published in | Journal of Geophysical Research Planets Vol. 117; no. E12 |
|---|---|
| Main Authors | , , , , , , , , , |
| Format | Journal Article |
| Language | English |
| Published |
Goddard Space Flight Center
Blackwell Publishing Ltd
01.12.2012
American Geophysical Union |
| Subjects | |
| Online Access | Get full text |
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| Abstract | The structure of Mercury's internal magnetic field has been determined from analysis of orbital Magnetometer measurements by the MESSENGER spacecraft. We identified the magnetic equator on 531 low-altitude and 120 high-altitude equator crossings from the zero in the radial cylindrical magnetic field component, Beta (sub rho). The low-altitude crossings are offset 479 +/- 6 km northward, indicating an offset of the planetary dipole. The tilt of the magnetic pole relative to the planetary spin axis is less than 0.8 deg.. The high-altitude crossings yield a northward offset of the magnetic equator of 486 +/- 74 km. A field with only nonzero dipole and octupole coefficients also matches the low-altitude observations but cannot yield off-equatorial Beta (sub rho) = 0 at radial distances greater than 3520 km. We compared offset dipole and other descriptions of the field with vector field observations below 600 km for 13 longitudinally distributed, magnetically quiet orbits. An offset dipole with southward directed moment of 190 nT-R-cube (sub M) yields root-mean-square (RMS) residuals below 14 nT, whereas a field with only dipole and octupole terms tuned to match the polar field and the low-altitude magnetic equator crossings yields RMS residuals up to 68 nT. Attributing the residuals from the offset-dipole field to axial degree 3 and 4 contributions we estimate that the Gauss coefficient magnitudes for the additional terms are less than 4% and 7%, respectively, relative to the dipole. The axial alignment and prominent quadrupole are consistent with a non-convecting layer above a deep dynamo in Mercury's fluid outer core. |
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| AbstractList | The structure of Mercury's internal magnetic field has been determined from analysis of orbital Magnetometer measurements by the MESSENGER spacecraft. We identified the magnetic equator on 531 low‐altitude and 120 high‐altitude equator crossings from the zero in the radial cylindrical magnetic field component,Bρ. The low‐altitude crossings are offset 479 ± 6 km northward, indicating an offset of the planetary dipole. The tilt of the magnetic pole relative to the planetary spin axis is less than 0.8°. The high‐altitude crossings yield a northward offset of the magnetic equator of 486 ± 74 km. A field with only nonzero dipole and octupole coefficients also matches the low‐altitude observations but cannot yield off‐equatorialBρ= 0 at radial distances greater than 3520 km. We compared offset dipole and other descriptions of the field with vector field observations below 600 km for 13 longitudinally distributed, magnetically quiet orbits. An offset dipole with southward directed moment of 190 nT‐RM3yields root‐mean‐square (RMS) residuals below 14 nT, whereas a field with only dipole and octupole terms tuned to match the polar field and the low‐altitude magnetic equator crossings yields RMS residuals up to 68 nT. Attributing the residuals from the offset‐dipole field to axial degree 3 and 4 contributions we estimate that the Gauss coefficient magnitudes for the additional terms are less than 4% and 7%, respectively, relative to the dipole. The axial alignment and prominent quadrupole are consistent with a non‐convecting layer above a deep dynamo in Mercury's fluid outer core.
Key Points
Mercury's magnetic field is an axialy aligned dipole offset 0.2 RM to the north
Additional high‐degree structure is less than 7% of the offset dipole
The result is consistent with a deep dynamo and a nonconvecting outer layer The structure of Mercury's internal magnetic field has been determined from analysis of orbital Magnetometer measurements by the MESSENGER spacecraft. We identified the magnetic equator on 531 low-altitude and 120 high-altitude equator crossings from the zero in the radial cylindrical magnetic field component, B. The low-altitude crossings are offset 479 ± 6 km northward, indicating an offset of the planetary dipole. The tilt of the magnetic pole relative to the planetary spin axis is less than 0.8°. The high-altitude crossings yield a northward offset of the magnetic equator of 486 ± 74 km. A field with only nonzero dipole and octupole coefficients also matches the low-altitude observations but cannot yield off-equatorial B = 0 at radial distances greater than 3520 km. We compared offset dipole and other descriptions of the field with vector field observations below 600 km for 13 longitudinally distributed, magnetically quiet orbits. An offset dipole with southward directed moment of 190 nT-RM3 yields root-mean-square (RMS) residuals below 14 nT, whereas a field with only dipole and octupole terms tuned to match the polar field and the low-altitude magnetic equator crossings yields RMS residuals up to 68 nT. Attributing the residuals from the offset-dipole field to axial degree 3 and 4 contributions we estimate that the Gauss coefficient magnitudes for the additional terms are less than 4% and 7%, respectively, relative to the dipole. The axial alignment and prominent quadrupole are consistent with a non-convecting layer above a deep dynamo in Mercury's fluid outer core. The structure of Mercury's internal magnetic field has been determined from analysis of orbital Magnetometer measurements by the MESSENGER spacecraft. We identified the magnetic equator on 531 low‐altitude and 120 high‐altitude equator crossings from the zero in the radial cylindrical magnetic field component, B ρ . The low‐altitude crossings are offset 479 ± 6 km northward, indicating an offset of the planetary dipole. The tilt of the magnetic pole relative to the planetary spin axis is less than 0.8°. The high‐altitude crossings yield a northward offset of the magnetic equator of 486 ± 74 km. A field with only nonzero dipole and octupole coefficients also matches the low‐altitude observations but cannot yield off‐equatorial B ρ = 0 at radial distances greater than 3520 km. We compared offset dipole and other descriptions of the field with vector field observations below 600 km for 13 longitudinally distributed, magnetically quiet orbits. An offset dipole with southward directed moment of 190 nT‐ R M 3 yields root‐mean‐square (RMS) residuals below 14 nT, whereas a field with only dipole and octupole terms tuned to match the polar field and the low‐altitude magnetic equator crossings yields RMS residuals up to 68 nT. Attributing the residuals from the offset‐dipole field to axial degree 3 and 4 contributions we estimate that the Gauss coefficient magnitudes for the additional terms are less than 4% and 7%, respectively, relative to the dipole. The axial alignment and prominent quadrupole are consistent with a non‐convecting layer above a deep dynamo in Mercury's fluid outer core. Mercury's magnetic field is an axialy aligned dipole offset 0.2 RM to the north Additional high‐degree structure is less than 7% of the offset dipole The result is consistent with a deep dynamo and a nonconvecting outer layer The structure of Mercury's internal magnetic field has been determined from analysis of orbital Magnetometer measurements by the MESSENGER spacecraft. We identified the magnetic equator on 531 low-altitude and 120 high-altitude equator crossings from the zero in the radial cylindrical magnetic field component, Beta (sub rho). The low-altitude crossings are offset 479 +/- 6 km northward, indicating an offset of the planetary dipole. The tilt of the magnetic pole relative to the planetary spin axis is less than 0.8 deg.. The high-altitude crossings yield a northward offset of the magnetic equator of 486 +/- 74 km. A field with only nonzero dipole and octupole coefficients also matches the low-altitude observations but cannot yield off-equatorial Beta (sub rho) = 0 at radial distances greater than 3520 km. We compared offset dipole and other descriptions of the field with vector field observations below 600 km for 13 longitudinally distributed, magnetically quiet orbits. An offset dipole with southward directed moment of 190 nT-R-cube (sub M) yields root-mean-square (RMS) residuals below 14 nT, whereas a field with only dipole and octupole terms tuned to match the polar field and the low-altitude magnetic equator crossings yields RMS residuals up to 68 nT. Attributing the residuals from the offset-dipole field to axial degree 3 and 4 contributions we estimate that the Gauss coefficient magnitudes for the additional terms are less than 4% and 7%, respectively, relative to the dipole. The axial alignment and prominent quadrupole are consistent with a non-convecting layer above a deep dynamo in Mercury's fluid outer core. |
| Audience | PUBLIC |
| Author | Slavin, James A. Solomon, Sean C. Johnson, Catherine L. Anderson, Brian J. Korth, Haje Borovsky, Joseph E. Zuber, Maria T. Winslow, Reka M. Purucker, Michael E. McNutt Jr, Ralph L. |
| Author_xml | – sequence: 1 givenname: Brian J. surname: Anderson fullname: Anderson, Brian J. email: brian.anderson@jhuapl.edu, brian.anderson@jhuapl.edu organization: Space Department, The Johns Hopkins University Applied Physics Laboratory, Laurel, Maryland, USA – sequence: 2 givenname: Catherine L. surname: Johnson fullname: Johnson, Catherine L. organization: Department of Earth and Ocean Sciences, University of British Columbia, Vancouver, British Columbia, Canada – sequence: 3 givenname: Haje surname: Korth fullname: Korth, Haje organization: Space Department, The Johns Hopkins University Applied Physics Laboratory, Laurel, Maryland, USA – sequence: 4 givenname: Reka M. surname: Winslow fullname: Winslow, Reka M. organization: Department of Earth and Ocean Sciences, University of British Columbia, Vancouver, British Columbia, Canada – sequence: 5 givenname: Joseph E. surname: Borovsky fullname: Borovsky, Joseph E. organization: Space Science Institute, Boulder, Colorado, USA – sequence: 6 givenname: Michael E. surname: Purucker fullname: Purucker, Michael E. organization: NASA Goddard Space Flight Center, Greenbelt, Maryland, USA – sequence: 7 givenname: James A. surname: Slavin fullname: Slavin, James A. organization: Department of Atmospheric, Oceanic and Space Sciences, University of Michigan, Ann Arbor, Michigan, USA – sequence: 8 givenname: Sean C. surname: Solomon fullname: Solomon, Sean C. organization: Department of Terrestrial Magnetism, Carnegie Institution of Washington, Washington, D. C., USA – sequence: 9 givenname: Maria T. surname: Zuber fullname: Zuber, Maria T. organization: Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, Massachusetts, USA – sequence: 10 givenname: Ralph L. surname: McNutt Jr fullname: McNutt Jr, Ralph L. organization: Space Department, The Johns Hopkins University Applied Physics Laboratory, Laurel, Maryland, USA |
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Aurnou, F. M. Al-Shamali, and N. Gomez Perez (2005), A numerical study of dynamo action as a function of spherical shell geometry, Earth Planet. Sci. Lett., 236, 542-557, doi:10.1016/j.epsl.2005.04.032. Stanley, S., and G. A. Glatzmaier (2010), Dynamo models for planets other than Earth, Space Sci. Rev., 152, 617-649, doi:10.1007/s11214-009-9573-y. Slavin, J. A., et al. (2012), MESSENGER observations of a flux-transfer-event shower at Mercury, J. Geophys. Res., 117, A00M06, doi:10.1029/2012JA017926. Solomon, S. C., R. L. McNutt Jr., R. E. Gold, and D. L. Domingue (2007), MESSENGER mission overview, Space Sci. Rev., 131, 3-39, doi:10.1007/s11214-007-9247-6. Giampieri, G., and A. Balogh (2002), Mercury's thermoelectric dynamo revisited, Planet. Space Sci. 50, 757-762. Alexeev, I. I., et al. (2010), Mercury's magnetospheric magnetic field after the first two MESSENGER flybys, Icarus, 209, 23-39, doi:10.1016/j.icarus.2010.01.024. Purucker, M. M., T. J. Sabaka, S. C. Solomon, B. J. 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McNutt Jr. (2012), Characteristics of the plasma distribution in Mercury's equatorial magnetosphere derived from MESSENGER Magnetometer observations, J. Geophys. Res., doi:10.1029/2012JA018052, in press. Wicht, J., M. Mandea, F. Takahashi, U. R. Christensen, M. Matushima, and B. Langlais (2007), The origin of Mercury's internal magnetic field, Space Sci. Rev., 132, 261-290, doi:10.1007/s11214-007-9280-5. Heyner, D., J. Wicht, N. Gómez-Pérez, D. Schmitt, H.-U. Auster, and K.-H. Glassmeier (2011b), Evidence from numerical experiments for a feedback dynamo generating Mercury's magnetic field, Science, 334, 1690-1693, doi:10.1126/science.1207290. Olson, P., and U. R. Christensen (2006), Dipole moment scaling for convection-driven planetary dynamos, Earth Planet. Sci. Lett., 250, 561-571, doi:101.1016/j.epsl.2006.08.008. Sundberg, T., et al. (2012), MESSENGER observations of dipolarization events in Mercury's magnetotail, J. Geophys. Res., 117, A00M03, doi:10.1029/2012JA017756. Slavin, J. A., et al. (2010), MESSENGER observations of extreme loading and unloading of Mercury's magnetic tail, Science, 329, 665-668, doi:10.1126/science.1188067. Takahashi, F., and M. Matsushima (2006), Dipolar and non-dipolar dynamos in thin spherical shell geometry with implications for the magnetic field of Mercury, Geophys. Res. Lett., 33, L10202, doi:10.1029/2006GL025792. Borovsky, J. E. (2012), Looking for evidence of mixing in the solar wind from 0.31 to 0.98 AU, J. Geophys. Res., 117, A06107, doi:10.1029/2012JA017525. Margot, J. L., S. J. Peale, R. F. Jurgens, M. A. Slade, and I. V. Holin (2007), Large longitude libration of Mercury reveals a molten core, Science, 316, 710-714, doi:10.1126/science.1140514. Christensen, U. R. (2006), A deep dynamo generating Mercury's magnetic field, Nature, 444, 1056-1058, doi:10.1038/nature05342. Ness, N. F., K. W. Behannon, R. P. Lepping, and Y. C. Whang (1975), The magnetic field of Mercury, 1, J. Geophys. 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Tsyganenko, S. C. Solomon, and R. L. McNutt Jr. (2004), Determination of the properties of Mercury's magnetic field by the MESSENGER mission, Planet. Space Sci., 52, 733-746, doi:10.1016/j.pss.2003.12.008. Smith, D. E., et al. (2012), Gravity field and internal structure of Mercury from MESSENGER, Science, 336, 214-217, doi:10.1126/science.1218809. Anderson, B. J., et al. (2010), The magnetic field of Mercury, Space Sci. Rev., 152, 307-339, doi:10.1007/s11214-009-9544-3. Anderson, B. J., C. L. Johnson, H. Korth, M. E. Purucker, R. M. Winslow, J. A. Slavin, S. C. Solomon, R. L. McNutt Jr., J. M. Raines, and T. H. Zurbuchen (2011), The global magnetic field of Mercury from MESSENGER orbital observations, Science, 333, 1859-1862, doi:10.1126/science.1211001. Aharonson, O., M. T. Zuber, and C. S. Solomon (2004), Crustal remanence in an internally magnetized non-uniform shell: A possible source for Mercury's magnetic field?, Earth Planet. Sci. 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(e_1_2_6_33_1) 1977; 42 e_1_2_6_19_1 e_1_2_6_13_1 e_1_2_6_36_1 e_1_2_6_11_1 e_1_2_6_34_1 e_1_2_6_17_1 e_1_2_6_15_1 e_1_2_6_38_1 e_1_2_6_43_1 e_1_2_6_20_1 e_1_2_6_41_1 e_1_2_6_9_1 e_1_2_6_5_1 e_1_2_6_7_1 e_1_2_6_24_1 e_1_2_6_49_1 e_1_2_6_3_1 e_1_2_6_22_1 e_1_2_6_28_1 e_1_2_6_45_1 e_1_2_6_26_1 e_1_2_6_47_1 e_1_2_6_52_1 e_1_2_6_10_1 e_1_2_6_31_1 e_1_2_6_50_1 Purucker M. E. (e_1_2_6_32_1) 2012; 43 e_1_2_6_14_1 e_1_2_6_35_1 e_1_2_6_12_1 e_1_2_6_18_1 e_1_2_6_39_1 e_1_2_6_16_1 e_1_2_6_37_1 e_1_2_6_42_1 e_1_2_6_21_1 e_1_2_6_40_1 e_1_2_6_8_1 e_1_2_6_4_1 e_1_2_6_6_1 e_1_2_6_25_1 e_1_2_6_48_1 e_1_2_6_23_1 e_1_2_6_2_1 e_1_2_6_29_1 e_1_2_6_44_1 e_1_2_6_27_1 e_1_2_6_46_1 |
| References_xml | – reference: Purucker, M. E., et al. (2012), Evidence for a crustal magnetic signature on Mercury from MESSENGER observations, Lunar Planet. Sci., 43, Abstract 1297. – reference: Slavin, J. A., et al. (2012), MESSENGER observations of a flux-transfer-event shower at Mercury, J. Geophys. Res., 117, A00M06, doi:10.1029/2012JA017926. – reference: Christensen, U. R. (2006), A deep dynamo generating Mercury's magnetic field, Nature, 444, 1056-1058, doi:10.1038/nature05342. – reference: Anderson, B. J., M. H. Acuña, D. A. Lohr, J. Scheifele, A. Raval, H. Korth, and J. A. Slavin (2007), The Magnetometer instrument on MESSENGER, Space Sci. Rev., 131, 417-450, doi:10.1007/s11214-007-9246-7. – reference: Stevenson, D. J. (1982), Reducing the non-axisymmetry of a planetary dynamo and an application to Saturn, Geophys. Astrophys. Fluid Dyn., 21, 113-127, doi:10.1080/03091928208209008. – reference: Alexeev, I. I., et al. (2010), Mercury's magnetospheric magnetic field after the first two MESSENGER flybys, Icarus, 209, 23-39, doi:10.1016/j.icarus.2010.01.024. – reference: Stanley, S., J. Bloxham, W. E. Hutchison, and M. T. Zuber (2005), Thin shell dynamo models consistent with Mercury's weak observed magnetic field, Earth Planet. Sci. Lett., 234, 27-38, doi:10.1016/j.epsl.2005.02.040. – reference: Bartels, J. (1936), The eccentric dipole approximating the Earth's magnetic field, J. Geophys. Res., 41, 225-250, doi:10.1029/TE041i003p00225. – reference: Olson, P., and U. R. Christensen (2006), Dipole moment scaling for convection-driven planetary dynamos, Earth Planet. Sci. Lett., 250, 561-571, doi:101.1016/j.epsl.2006.08.008. – reference: Purucker, M. M., T. J. Sabaka, S. C. Solomon, B. J. Anderson, H. Korth, M. T. Zuber, and G. A. Neumann, (2009), Mercury's internal magnetic field: Constraints on large- and small-scale fields of crustal origin, Earth Planet. Sci. Lett., 285, 340-346, doi:10.1016/j.epsl.2008.12.017. – reference: Ness, N. F., K. W. Behannon, R. P. Lepping, and Y. C. Whang (1975), The magnetic field of Mercury, 1, J. Geophys. Res., 80, 2708-2716, doi:10.1029/JA080i019p02708. – reference: Stanley, S., and A. Mohammadi (2008), Effects of an outer thin stably stratified layer on planetary dynamos, Phys. Earth Planet. Inter., 168, 179-190, doi:10.1016/j.pepi.2008.06.016. – reference: Glassmeier, K.-H., H.-U. Auster, and U. Motschmann (2007a), A feedback dynamo generating Mercury's magnetic field, Geophys. Res. Lett., 34, L22201, doi:10.1029/2007GL031662. – reference: Gómez-Pérez, N., and J. Wicht (2010), Behavior of planetary dynamos under the influence of external magnetic fields: Application to Mercury and Ganymede, Icarus, 209, 53-62, doi:10.1016/j.icarus.2010.04.006. – reference: Heimpel, M., J. M. Aurnou, F. M. Al-Shamali, and N. Gomez Perez (2005), A numerical study of dynamo action as a function of spherical shell geometry, Earth Planet. Sci. Lett., 236, 542-557, doi:10.1016/j.epsl.2005.04.032. – reference: Gómez-Pérez, N., and S. C. Solomon (2010), Mercury's weak magnetic field: A result of magnetospheric feedback?, Geophys. Res. Lett., 37, L20204, doi:10.1029/2010GL044533. – reference: Anderson, B. J., M. H. Acuña, H. Korth, M. E. Purucker, C. L. Johnson, J. A. Slavin, S. C. Solomon, and R. L. McNutt Jr. (2008), The magnetic field of Mercury: New constraints on structure from MESSENGER, Science, 321, 82-85, doi:10.1126/science.1159081. – reference: Smith, D. E., et al. (2012), Gravity field and internal structure of Mercury from MESSENGER, Science, 336, 214-217, doi:10.1126/science.1218809. – reference: Ness, N. F., K. W. Behannon, R. P. Lepping, Y. C. Whang, and K. H. Schatten (1974), Magnetic field observations near Mercury: Preliminary results, Science, 185, 151-160, doi:10.1126/science.185.4146.151. – reference: Shue, J.-H., J. K. Chao, H. C. Fu, C. T. Russell, P. Song, K. K. Khurana, and H. J. Singer (1997), A new functional form to study the solar wind control of the magnetopause size and shape, J. Geophys. Res., 102, 9497-9511, doi:10.1029/97JA00196. – reference: Solomon, S. C., R. L. McNutt Jr., R. E. Gold, and D. L. Domingue (2007), MESSENGER mission overview, Space Sci. Rev., 131, 3-39, doi:10.1007/s11214-007-9247-6. – reference: Winslow, R. M., C. L. Johnson, B. J. Anderson, H. Korth, J. A. Slavin, M. E. Purucker, and S. C. Solomon (2012), Observations of Mercury's northern cusp region with MESSENGER's Magnetometer, Geophys. Res. Lett., 39, L08112, doi:10.1029/2012GL051472. – reference: Uno, H., C. L. Johnson, B. J. Anderson, H. Korth, and S. C. Solomon (2009), Mercury's internal magnetic field: Constraints from regularized inversions, Earth Planet. Sci. Lett., 285, 328-339, doi:10.1016/j.epsl.2009.02.032. – reference: Zurbuchen, T. H., et al. (2011), MESSENGER observations of the spatial distribution of planetary ions near Mercury, Science, 333, 1862-1865, doi:10.1126/science.1211302. – reference: Korth, H., B. J. Anderson, M. H. Acuña, J. A. Slavin, N. A. Tsyganenko, S. C. Solomon, and R. L. McNutt Jr. (2004), Determination of the properties of Mercury's magnetic field by the MESSENGER mission, Planet. Space Sci., 52, 733-746, doi:10.1016/j.pss.2003.12.008. – reference: Stevenson, D. J. (1987), Mercury's magnetic field-A thermoelectric dynamo?, Earth Planet. Sci. Lett., 82, 114-120, doi:10.1016/0012-821X(87)90111-7. – reference: Heyner, D., D. Schmitt, K.-H. Glassmeier, and J. Wicht (2011a), Dynamo action in an ambient field, Astron. Nachr., 332, 36-42, doi:10.1002/asna.201011466. – reference: Borovsky, J. E. (2012), Looking for evidence of mixing in the solar wind from 0.31 to 0.98 AU, J. Geophys. Res., 117, A06107, doi:10.1029/2012JA017525. – reference: Cao, H., C. T. Russell, U. R. Christensen, M. K. Dougherty, and M. E. Burton (2011), Saturn's very axisymmetric magnetic field: No detectable secular variation or tilt, Earth Planet. Sci. Lett., 304, 22-28, doi:10.1016/j.epsl.2011.02.035. – reference: Sundberg, T., et al. (2012), MESSENGER observations of dipolarization events in Mercury's magnetotail, J. Geophys. Res., 117, A00M03, doi:10.1029/2012JA017756. – reference: Wicht, J., M. Mandea, F. Takahashi, U. R. Christensen, M. Matushima, and B. Langlais (2007), The origin of Mercury's internal magnetic field, Space Sci. Rev., 132, 261-290, doi:10.1007/s11214-007-9280-5. – reference: Takahashi, F., and M. Matsushima (2006), Dipolar and non-dipolar dynamos in thin spherical shell geometry with implications for the magnetic field of Mercury, Geophys. Res. 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Wicht (2008), Models of magnetic field generation in partly stable planetary cores: Applications to Mercury and Saturn, Icarus, 196, 16-34, doi:10.1016/j.icarus.2008.02.013. – reference: Johnson, C. L., et al. (2012), MESSENGER observations of Mercury's magnetic field structure, J. Geophys. Res., doi:10.1029/2012JE004217, in press. – reference: Stevenson, D. J. (2003), Planetary magnetic fields, Earth Planet. Sci. Lett., 208, 1-11, doi:10.1016/S0012-821X(02)01126-3. – reference: Korth, H., B. J. Anderson, C. L. Johnson, R. M. Winslow, J. A. Slavin, M. E. Purucker, S. C. Solomon, and R. L. McNutt Jr. (2012), Characteristics of the plasma distribution in Mercury's equatorial magnetosphere derived from MESSENGER Magnetometer observations, J. Geophys. Res., doi:10.1029/2012JA018052, in press. – reference: Anderson, B. J., C. L. Johnson, H. Korth, M. E. Purucker, R. M. Winslow, J. A. Slavin, S. C. Solomon, R. L. McNutt Jr., J. M. Raines, and T. H. Zurbuchen (2011), The global magnetic field of Mercury from MESSENGER orbital observations, Science, 333, 1859-1862, doi:10.1126/science.1211001. – reference: Aharonson, O., M. T. Zuber, and C. S. Solomon (2004), Crustal remanence in an internally magnetized non-uniform shell: A possible source for Mercury's magnetic field?, Earth Planet. Sci. Lett., 218, 261-268, doi:10.1016/S0012-821X(03)00682-4. – reference: Manglik, A., J. Wicht, and U. R. Christensen (2010), A dynamo model with double diffusive convection for Mercury's core, Earth Planet. Sci. Lett., 289, 619-628, doi:10.1016/j.epsl.2009.12.007. – reference: Glassmeier, K.-H., J. Grosser, U. Auster, D. Constantinescu, Y. Narita, and S. Stellmach (2007b), Electromagnetic induction effects and dynamo action in the Hermean system, Space Sci. Rev., 132, 511-527, doi:10.1007/s11214-007-9244-9. – reference: Heyner, D., J. Wicht, N. Gómez-Pérez, D. Schmitt, H.-U. Auster, and K.-H. Glassmeier (2011b), Evidence from numerical experiments for a feedback dynamo generating Mercury's magnetic field, Science, 334, 1690-1693, doi:10.1126/science.1207290. – reference: Margot, J. L., S. J. Peale, R. F. Jurgens, M. A. Slade, and I. V. Holin (2007), Large longitude libration of Mercury reveals a molten core, Science, 316, 710-714, doi:10.1126/science.1140514. – reference: Alexeev, I. I., E. S. Belenkaya, S. Y. Bobrovnikov, J. A. Slavin, and M. Sarantos (2008), Paraboloid model of Mercury, J. Geophys. Res., 113, A12210, doi:10.1029/2008JA013368. – reference: Anderson, B. J., et al. (2010), The magnetic field of Mercury, Space Sci. Rev., 152, 307-339, doi:10.1007/s11214-009-9544-3. – reference: Korth, H., B. J. Anderson, J. M. Raines, J. A. Slavin, T. H. Zurbuchen, C. L. Johnson, M. E. Purucker, R. M. Winslow, S. C. Solomon, and R. L. McNutt Jr. (2011), Plasma pressure in Mercury's equatorial magnetosphere derived from MESSENGER Magnetometer observations, Geophys. Res. 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| Snippet | The structure of Mercury's internal magnetic field has been determined from analysis of orbital Magnetometer measurements by the MESSENGER spacecraft. We... |
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| Title | Low-degree structure in Mercury's planetary magnetic field |
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