The origin of the compressional stresses that formed Hinks Dorsum is not well understood. Surveys of tectonic features on Eros show only a few sets of structures radial to impact or other features [Prockter et al., 2002; Thomas et al., 2002b; Buczkowski et al., 2008]. Impact craters with squared outlines, however, are cited as evidence of structural control [Cheng et al., 2002; Prockter et al., 2002]. The global distribution of grooves, troughs, and ridges on Eros suggests a pervasive fabric of fractures [Prockter et al., 2002; Thomas et al., 2002b], supporting the interpretation that the asteroid is a coherent body held together by material strength rather than by gravitational attraction alone [Zuber et al., 2000; Prockter et al., 2002; Thomas et al., 2002b]. Proposed expressions of this fabric are a Calisto Fossae-Hinks Dorsum plane and a prominent facet of Eros [see Thomas et al., 2002b]. Our analysis indicates that the dip of the Hinks Dorsum fault is not along these planes and thus the fault was likely not influenced by the putative fabric. This does not exclude the possibility that the Hinks Dorsum fault exploited another preexisting zone of weakness, conjugate to the Calisto and surface facet planes.
 The stress necessary to initiate thrust faulting on Eros is determined by its near-surface strength. Two approaches are used to evaluate the near-surface shear strength of the asteroid, frictional strength and rock mass strength. The frictional strength is controlled by the resistance to brittle failure by sliding on randomly oriented, through going fractures (Byerlee's law). In terms of the maximum σ1 and minimum σ3 principal effective stresses Byerlee's law is expressed by σ1 ≃ 5σ3 for σ3 < 110 MPa where σ3 = ρgz and ρ is the density, g acceleration due to gravity, and z is the depth [see Brace and Kohlstedt, 1980]. Although g on Eros varies from 0.24 to 0.56 cm s−2 [Veverka et al., 2001a], 0.5 cm s−2 is a good average in the area of Hinks Dorsum [see Robinson et al., 2001, Figure 2]. Using the mean density of Eros ρ = 2.67 g/cm2 [Veverka et al., 2000], the shear strength at a depth of 0.25 km is ∼1.3 MPa (Figure 3). The frictional strength criteria is a lower limit on the shear strength for near-surface rocks because it assumes the cohesion Co = 0 [see Schultz, 1993; Scholz, 2002]. The strength of near-surface rocks with non-zero cohesion is better represented by the Hoek-Brown failure criterion given by
where σ1 and σ3 are the effective principal stresses, σc is the uniaxial compressive strength of intact rock, and m, s, and a are material constants related to the Geologic Strength Index (GSI) and a rock mass disturbance factor d [Hoek et al., 2002; Hoek and Diederichs, 2006]. Using σc = 200 MPa, the mean compressive strength of intact stony meteorites [Petrovic, 2001], a GSI = 45 (consistent with highly jointed basalt rock mass), and d = 1.0 (where 0 = undisturbed, 1 = very disturbed) [Hoek et al., 2002], the shear strength at a depth of 0.25 km is ∼6 MPa (Figure 3). Based on these two approaches, we estimate the near-surface shear strength of Eros to be from ∼1 to 6 MPa. This shear strength is well above the maximum expected from tidally induced stresses [e.g., Dobrovolskis, 1982] and far exceeds recent estimates of the strength of Phobos, Pandora, and Epimetheus (0.01 to 0.1 MPa) [Morrison et al., 2009]. Thermally induced stresses could exceed 5 MPa [Dombard and Freed, 2002], however, the presence of a relatively thick, uncompacted regolith [Veverka et al., 2001b; Robinson et al., 2002; Thomas and Robinson, 2005] will likely insolate the interior from their effects. The most likely source of stress capable of forming thrust faults on Eros is impact-induced compression [Melosh, 1989; Richardson et al., 2004; Thomas et al., 2001].
 The relatively young impact crater Shoemaker (there is no IAU approved name for this crater), which contains Charlois Regio, is ∼7.6 km in diameter and is superposed on the rim of the larger Himeros crater [Thomas et al., 2002a; Thomas and Robinson, 2005]. The relatively young age of both Shoemaker crater and Hinks Dorsum, combined with the likely need for impact-induced stress in the formation of Hinks, raises the question of a possible genetic relation. Shoemaker has been associated with most of the large ejecta blocks on Eros [Thomas et al., 2001], and has removed much of the population of craters <0.5 km in diameter within ∼9 km straight line distance of the center of Shoemaker [Thomas and Robinson, 2005]. A global structural feature map of Eros shows that Hinks Dorsum is roughly circumferential to the center of Shoemaker [see Thomas et al., 2002b, Figure 1], and the northward thrust slip direction of the fault is away from the crater center. Following the approach of Thomas and Robinson , the straight-line distance from the center of Shoemaker to points along Hinks Dorsum are plotted (Figure 4a). The plot indicates that Hinks Dorsum has a simple geometric relation to Shoemaker crater. Over half its length is within a very narrow range of distance from the center of Shoemaker (∼8.3 to 8.6 km), with a maximum distance of ∼10.3 km at the eastern end of the structure (Figure 4a). While the loss of craters within a certain distance of Shoemaker can be related to a level of impact induced acceleration or energy deposition, the formation of a thrust fault at a near-constant distance may have involved compressional stresses that exceeded 6 MPa. We note that segments of Hinks Dorsum are very close to the transition from low to high crater density, particularly in Himeros (Figure 4b). This spatial correlation suggests that the Hinks Dorsum thrust faults acted as a mechanical discontinuity where seismic shaking was attenuated. The crater density effects reach ∼9 km from Shoemaker around the entire asteroid, so any discontinuity at Hinks is not the only control on the crater density transition. Impact-induced compression from the Shoemaker event may have formed the Hinks Dorsum thrust fault, and subsequent seismic shaking likely resulted in the additional slip on the fault and the growth of the structure.