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Laser Altimeter Observations from Messengerls First Mercury Flyby

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Laser Altimeter Observations from Messengerls First Mercury Flyby SPECIALSECTION limited by the resolution of the timing electronics. REPORT The radial accuracy of ~100 m is limited by uncer- tainties in the trajectory associated with errors in the ephemerides of MESSENGER and Mercury. Laser Altimeter Observations from The profile spans ~ 20% of the circumference of the planet and shows a 5.2-km dynamic range MESSENGER’s First Mercury Flyby of topography and 930-m root-mean-square (RMS) roughness (Fig. 1). The radius of Mercury Maria T. Zuber,1* David E. Smith,2 Sean C. Solomon,3 Roger J. Phillips,4 Stanton J. Peale,5 apparently decreases by 1.4 km along the equator James W. Head III,6 Steven A. Hauck II,7 Ralph L. McNutt Jr.,8 Jürgen Oberst,9 from ~10° to 90° E, corresponding to a 0.02° GregoryA.Neumann,2 Frank G. Lemoine,2 Xiaoli Sun,2 Olivier Barnouin-Jha,8 John K. Harmon10 downward slope to the east. This long-wavelength surface tilt begins 30° west of the previously esti- A 3200-kilometers-long profile of Mercury by the Mercury Laser Altimeter on the MESSENGER mated COF/COM offset (6) and was not sampled spacecraft spans ~20% of the near-equatorial region of the planet. Topography along the profile is in Earth-based radar altimetry (4). Such a long- characterized by a 5.2-kilometer dynamic range and 930-meter root-mean-square roughness. At wavelength slope, if a fundamental feature of the long wavelengths, topography slopes eastward by 0.02°, implying a variation of equatorial shape equatorial shape of the planet, might arise from that is at least partially compensated. Sampled craters on Mercury are shallower than their crustal thickness or crustal density variations, global- counterparts on the Moon, at least in part the result of Mercury’s higher gravity. Crater floors vary scale mantle density variations, or topography along in roughness and slope, implying complex modification over a range of length scales. the planet’s core-mantle boundary, which for Mercury is ~600 km beneath the surface. opography is a fundamental measurement that was in darkness during the flyby, and within The slope can be interpreted in the context of to characterize quantitatively the surfaces the hemisphere not imaged by Mariner 10. Con- an ellipsoidal planetary shape (10). If we suppose Tof solid planetary bodies at length scales sequently, there are no optical images of the re- that the difference in principal moments of in- ranging from the long-wavelength shape to such gion in which altimetry was collected, so we used ertia, B – A, is entirely a result of an ellipsoidal local and regional processes as impact cratering, an Arecibo radar image (8) to correlate the profile distribution of surface mass with density rs and volcanism, and faulting. During the first flyby with surface features. The MLA began ranging with semi-axes a>b>c,then ’ of Mercury by the MESSENGER spacecraft on ~1 min before the spacecraft s closest approach ÀÁ 4 4prsabc 8prsR 14 January 2008 (1), the Mercury Laser Altimeter and continued for ~10 min. Usable returns were B − A ¼ a2 − b2 ≈ ðÞða − b 1Þ (MLA) (2, 3) successfully ranged to the planet’s received up to an altitude of 1500 km, which was 15 15 surface, providing the first altimetric observations larger than the expected maximum of 1200 km from which we may write of the planet from a spacecraft. (2). As the spacecraft velocity and range from B − A C C 〈r〉 a − b ¼ 5 R m ð Þ Previous measurements of the shape and to- Mercury changed during the flyby, the size of 2 2 2 Cm C MR rs pography of Mercury had been derived from laser spots on the surface varied from 23 to 134 m Earth-based radar ranging (4, 5) constrained by and the shot spacing varied from 888 to 725 m (9). where A<B<Care the principal moments of range observations from Mariner 10 (6). Because The vertical precision varied with the received inertia of Mercury, Cm is the moment of of the low inclination (7°) of Mercury’s orbital signal strength and is <15 cm at the closest range, inertia of the mantle and crust alone, and M, plane to the ecliptic, Earth-based altimetric profiles are limited to ±12° latitude and have a spatial resolution of ~6 × 100 km2 and a vertical precision of 100 m (5). These observations indicated a planetary reference radius of 2440 ± 1 km, an equatorial ellipticity of 540 ± 54 ×10−6,andan equatorial center of figure (COF) offset from the planet’s center of mass (COM) of 640 ± 78 m in the direction 319.5° ± 6.9° W (6, 7). The MLA profile (Fig. 1) was acquired ap- proximately along Mercury’s equator, in a region 1Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139–4307, USA. 2Solar System Exploration Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA. 3Department of Terrestrial Magnetism, Carnegie Institution of Washington, Washington, DC 20015, USA. 4Southwest Research Institute, Boulder, CO 80302, USA. 5Department of Physics, University of California, Santa Barbara, CA 93106, USA. 6Department of Geological Sciences, Brown University, Providence,RI02912,USA.7Department of Geological Sciences, Case Western Reserve University, Cleveland, OH 44106, USA. 8Johns Hopkins University Applied Physics 9 Fig. 1. (Top) MLA profile (vertical exaggeration 105:1). (Bottom) Arecibo radar image [adapted Laboratory, Laurel, MD 20723, USA. Institute of Planetary 8 Research, German Aerospace Center (DLR), Berlin, D-12489 from ( )] with MLA profile location (white line) superposed. Arrows at top indicate locations of Germany. 10National Astronomy and Ionosphere Center, craters in Table 1 interpreted from detailed analysis of MLA profile points. The locations of several Arecibo Observatory, Arecibo 00612, Puerto Rico. of the major craters are indicated by arrows on the radar image. The two-ringed circular structure *To whom correspondence should be addressed. E-mail: in the Arecibo image at ~55 to 60°E is represented in part by a deep depression in the altimetry, [email protected] but north-south radar ambiguities may be contributing to the structure in the image. www.sciencemag.org SCIENCE VOL 321 4 JULY 2008 77 MESSENGER Table 1. Crater apparent slopes, RMS roughness, and pulse widths. Apparent Emission Apparent RMS Spot Longitude floor Range angle† floor slope‡ roughness Pulse width (ns) roughness§ (oE) diameter* (km) (deg) (deg) (m) (m) (km) 21.1–22.4 55.3 415 61 0.298 89.8 5.0 ± 2.1 0.3 ± 0.7 33.7–33.9 8.5 293 49 –0.451 11.8 12.4 ± 1.8 1.8 ± 3.4 35–35.3 12.8 289 48 1.26 24.3 14.6 ± 10.8 2.3 ± 2.4 38.5–38.9 17 285 44 –0.571 46.3 22.5 ± 18.4 3.8 ± 3.9 42.9–43.2 12.8 293 40 0.252 20.3 12.0 ± 10.6 1.5 ± 2.1 44.5–44.6 4.3 298 38 –0.573 7.9 19.6 ± 20.7 2.9 ± 4.0 46–47.3|| 55.4 313 36 0.177 66.5 19.3 ± 14.5 2.8 ± 2.7 48.8–50.6|| 76.7 336 34 –0.0784 31.9 20.9 ± 15.3 3.0 ± 2.7 52.3–52.4 4.3 365 31 0.117 5.7 18.0 ± 16.4 2.4 ± 2.9 56.8–59.1 98 429 26 0.0852 96.5 20.6 ± 16.7 2.7 ± 2.8 81–82.3 55.4 1020 1.5 –0.0008 110 6.3 ± 2.1 0.2 ± 0.3 *Length of MLA-crossing chord. †Emission angle is the angle between the range vector and surface normal. ‡Positive slopes are defined to be downward to the west. §Roughness from pulse width corrected for spacecraft range and emission angle. ||Craters shown in Fig. 2. Fig. 2. Close-up of two cra- 2 are complex and do not operate uniformly over ters showing contrast in floor different length scales. Potential sources of mod- roughness and tilt. The ver- ification include anelastic relaxation, volcanic re- tical exaggeration is 30:1. 0 surfacing, tectonic subsidence, wall slumping, and ejecta emplacement from younger nearby im- pacts, and the variability implies that a combina- Elevation, km -2 50 km tion of these processes operated on the profiled 44 46 48 50 52 54 craters. Longitude,oE R, and <r> are the mass, radius, and mean have diameters (107 km and 122 km) comparable References and Notes 1. S. C. Solomon et al., Science 321, 59 (2008). density of Mercury, respectively. The form of to that of Tycho (102 km), among the largest 2. J. F. Cavanaugh et al., Space Sci. Rev. 131, 451 (2007). the right hand side of Eq. (2) is convenient fresh craters on the Moon’s nearside (Fig. 2). 3. The MLA is a time-of-flight laser rangefinder that uses because from measurements we have (B – A)/Cm Whereas Tycho has a depth of 4.8 km (15), these direct detection and pulse-edge timing to determine −4 11 precisely the range from the MESSENGER spacecraft to = (2.03 ± 0.12) × 10 ( ), and from models we craters have depths of 2.4 and 2.9 km, respec- ’ C /C C/MR2 the target surface. MLA s laser transmitter emits have m = 0.4 to 0.7 and =0.31to tively. Although these craters may have under- 5-ns-wide pulses at an 8-Hz rate with 20 mJ of energy at 0.35 (12, 13).
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