by: Charles O’Dale
- Type: Simple
- Age: <1,130 yearsa – HOLOCENE
- Diameter: 36m
- Depth: 6m
- Location: N 53° 59.95’ W 115° 35.85’
- Shock Metamorphism: shock effects are limited to planar microstructures (PMs) observed in quartz grains and Fe-Ni oxide spherules
a Dating Method: 14C dating of charcoal buried by impact ejecta. (Herd et al 2008)
- Gillian Sullivan & Chuck O’Dale – exploration of the Whitecourt Impact Crater presented at the Ottawa Centre, RASC.
- Crater Investigation Study – Image Library
Whitecourt Crater Investigation Summary
|Atmospheric Entry Parameters:|
|Radius*||0.35m to 0.40m|
|Velocity*||12km/s to 16km/s|
|Entry Angle*||41° to 56°|
|Radius*||0.25m to 0.33m|
|Velocity||8km/s to 10km/s|
|Impact Angle||40° to 55°|
|Direction of Flight||060° to 075° true|
|Final Crater Diameter||36m|
|Final Crater Depth**1||6m|
|Transient Crater Diameter||~29m|
|Maximum Transient Crater Depth***||~10.5m|
|Meteorite Type2||IIIAB Iron Medium Octahedrite|
* Based on modeling
** As measured parallel to the local hill slope
*** Considering the depth of the transient crater boundary below the 6m crater depth
1,2 Herd et al. (2008)
Randolf S. KOFMAN, Christopher D. K. HERD, Duane G. FROESE
Abstract– The <1,100 yr old Whitecourt meteorite impact crater, located south of Whitecourt, Alberta, Canada, is a well-preserved bowl-shaped structure having a depth and diameter of approximately 6 and 36 m, respectively. There are fewer than a dozen known terrestrial sites of similar size and age. Unlike most of these sites, however, the Whitecourt crater contains nearly all of the features associated with small impact craters including meteorites, ejecta blanket, observable transient crater boundary, raised rim, and associated shock indicators. This study indicates that the crater formed from the impact of an approximately 1 m diameter type IIIAB iron meteoroid traveling east-northeast at less than approximately 10 km s−1, striking the surface at an angle between 40° and 55° to horizontal. It appears that the main mass survived atmospheric transit relatively intact, with fragmentation and partial melting during impact. Most meteoritic material has a jagged, shrapnel-like morphology and is distributed downrange of the crater.
The <1,100 yr old Whitecourt meteorite impact crater, located south of Whitecourt, Alberta, Canada, is a well-preserved bowl-shaped structure having a depth and diameter of approximately 6 and 36 m, respectively. There are fewer than a dozen known terrestrial sites of similar size and age. Unlike most of these sites, however, the Whitecourt crater contains nearly all of the features associated with small impact craters including meteorites, ejecta blanket, observable transient crater boundary, raised rim, and associated shock indicators. This study indicates that the crater formed from the impact of an approximately 1 m diameter type IIIAB iron meteoroid traveling east-northeast at less than approximately 10 km/s, striking the surface at an angle between 40° and 55° to horizontal. It appears that the main mass survived atmospheric transit relatively intact, with fragmentation and partial melting during impact. Most meteoritic material has a jagged, shrapnel-like morphology and is distributed downrange of the crater (Kofman et al – Meteoritics & Planetary Science 2010). Target sediments consist of Quaternary glacial deposits.
Local hunters had used this unusual “hole in the ground” south of the town of Whitecourt as a meeting point for many years. Deer could often be found drinking rainwater that collected in the bottom of the crater. It was in July 2007 that local residents contacted Dr. Chris Herd, the curator of the Alberta Meteorite Collection and a meteorite researcher at the University of Alberta, after recovering several metallic fragments next to this large asymmetric hole in the ground. Analysis of one of the fragments with a scanning electron microscope (SEM) verified that it was a meteorite. This, and follow-up field work, confirmed that the well known structure was indeed an impact crater.
The crater contains nearly all the features similar to other Barringer type (simple) bowl-shaped craters. This includes meteorites, an ejecta blanket, an observable transient crater boundary, a raised rim, and a number of associated shock indicators. The shock effects are limited to planar microstructures (PMs) observed in quartz grains and Fe-Ni oxide spherules. Evidence of target sediment melting has not been found. A raised rim, which typically circumnavigates simple craters, only extends between the bearings ~020° and ~110°; the opposing side of the crater shows little evidence of uplift. Surface contours within the crater are relatively circular and evenly spaced indicating that there has been no preferential crater wall steepening. There is a slight shift along the south wall that appears to be in response to creep (Kofman et al, 2010).
A) Bare-Earth LiDAR image of the crater and nearby surroundings. B) Surface contours at 1 m intervals. (Kofman et al – Meteoritics & Planetary Science 2010)
Proximal ejecta located at the first sample site southwest of the crater rim along the A–A′ . The horizons indicated are disturbed, and represent sediment from which the ejecta was derived.
Combined results of two magnetic surveys performed using the GEM Systems GSM 19-TW. This represents the diurnally corrected data. Dense vegetation along the southern half of the grid made surveying slightly more difficult. A large magnet was found at the large positive anomaly on the NW crater rim (one of three found to date, likely left behind by meteorite hunters). With the exception of the magnet, large meteorites, about several hundred grams each, were found at all the major anomalies. Several other meteorites of similar scale were recovered from additional localized anomalies evident only in the raw data.
An option of the 2012 RASC General Assembly (GA) in Edmonton was a post-conference field trip to the Whitecourt Crater guided by Dr. Herd. The crater is just south of the town of Whitecourt, a two hour bus ride away from the GA site in Edmonton. It was a “no brainer” that Gillian and I were going to be on that expedition.
From the bus “drop off point”, a guided hike of over a couple of kilometres brought us to the rim of the crater. It was worth the sweat.
The Impacting Meteorite
The Whitecourt impacting meteorite is identified as a medium octahedrite (Om) IIIAB that was derived 4.5 billion years ago from the core of a >50 km diameter asteroid. From the analysis of the widmanstatten patterns (Goldstein 1964) within the Whitecourt meteorites, it was determined that the core of this asteroid cooled at a rate of 50°C per million years.
The Whitecourt Crater morphology, lack of a large buried meteoroid mass, meteorite morphology, meteorite dust, and Fe-Ni oxide spherules suggest the main mass of the meteoroid was completely disrupted on impact and that this was a hypervelocity event of >4 km/s (Kofman et al, 2010).
Most meteoroids retain their hypervelocities and completely vaporize in an explosion when they impact the earth. In some cases the earth’s atmosphere slows the meteoroids to terminal velocity so they are relatively intact meteorites upon impact. These meteorites have rounded edges with regmaglypts. Regmaglypts are thumbprint-like depressions caused by the uneven flow of air during passage through the atmosphere and the consequent surface melting and ablation.
The smaller size of the Whitecourt hypervelocity impactor (approximately 1 metre diameter upon impact) is unusual as there are surviving meteorites elsewhere several times larger than this that did not cause an explosive (E = 1/2 mv²) type crater. These larger meteoroids for some reason completely lost their hypervelocities in the atmosphere and impacted at terminal velocity without causing the 1/2 mv² explosion. In contrast, this relatively small Whitecourt meteorite retained enough energy to explode on contact vaporizing much of the original meteoroid and forming the crater and associated shrapnel (from a conversation with Dr. C. Herd).
The Whitecourt impact event produced octahedrite meteorites having two different post impact shapes.
Some of the meteorites have sharp “shrapnel-type” edges. The hypothesis is that most of the meteorite was vaporized upon hyper-velocity impact, but on contact, some parts were ejected in the explosion as shrapnel before the main body was vaporized.
Other meteorites found at the site have the rounded edges with regmaglypts. These meteorites broke away from the main body while still in the atmosphere and impacted around the crater at terminal velocity.
From: The Results of the Investigation of the Whitecourt Crater (Alberta, Canada) Randolf S. Kofman* University of Alberta, Edmonton, Alberta, Canada firstname.lastname@example.org and C. D. K. Herd University of Alberta, Edmonton, Alberta, Canada and D. G. Froese University of Alberta, Edmonton, Alberta, Canada
It is possible to place constraints on the Whitecourt meteoroid’s trajectory (direction of flight and impact angle) and impact velocity. For the direction of flight we can consider the crater morphology, ejecta blanket distribution and meteorite distribution. Both the ejecta blanket and meteorite distributions show rough bilateral symmetry along a trend of 065° to 075°. Additionally, both features show clear concentrations along this orientation. We propose that the meteorite distribution formed in response to the main mass fragmenting during impact and the resultant shrapnel scattering downrange forming a ‘shrapnel field,’ or ‘spall field.’ These two observations indicate that the meteoroid was traveling towards the east-northeast when it struck the surface. The crater morphology supports this hypothesis. A raised rim, observed to be restricted to between 020° and 110°, is expected downrange, and a depressed rim uprange at impact angles between ~40° and 45°, as is observed at the Whitecourt Crater [e.g. Herrick & Forsberg-Taylor, 2003]. For the impact angle we can consider distribution of the ejecta blanket in combination with the aforementioned observations of Herrick & Forsberg-Taylor (2003). On airless bodies a shift from an axially symmetric distribution to a bilaterally symmetric distribution concentrated down range occurs as low as ~45° to the target surface, with an uprange forbidden zone developing as the impact angle drops below 45° [Gault & Wedekind, 1978; Shultz, 1992c; Melosh, 1989]. The ejecta blanket concentrates downrange at higher angles and the forbidden zone develops at lower angles in the presence of an atmosphere [Herrick & Forsberg-Taylor, 2003; Shultz, 1992c]. Together the location of the raised rim and distribution of the ejecta blanket suggest that the impact angle was likely between 40° and 55°. Constraints on the impact velocity are somewhat more tenuous. The observed lack of significant impactor melting and complete lack of target sediment melting suggest that it is lower than the 12 km/s to 15 km/s velocities proposed for the Meteor Crater, Arizona impact [Artemieva & Pierazzo, 2009; Melosh & Collins, 2005]. In addition, the crater morphology, lack of a large buried mass, meteorite morphology, meteorite dust, and Fe-Ni oxide spherules suggest the main mass was completely disrupted on impact and that this was a hypervelocity event. We propose an impact velocity of roughly 8 km/s to 10 km/s.
In order to complete our exploration of the Whitecourt Crater, Gillian and I flew our bird, C-GOZM, to the precise coordinates of the crater stored in the GPS. Little did we know how invisible the site is from low altitude. We could not see the crater at all while flying over the coordinates (while concentrating on not hitting anything!). All we could do was aim the wing at the GPS location, take the images and hope for the best.
The image above shows the crater under the wing. See it? ….. Neither do I !
Give up? … The image below illustrates the crater location.
[see – METEORITE]
Brent Dalrymple, Radiometric Dating Does Work! Reports of the National Center for Science Education
Goldstein J.L., Ogilvie, R.E., The Growth of the Widmanstatten Pattern in Metallic Meteorites. Smithsonian Astrophysical Observatory, Cambridge Mass, 30 OCT 1964.
Kofman R.S., Herd C.D.K., Froese D.G., The Whitecourt meteorite impact crater, Alberta, Canada. Meteoritics & Planetary Science 1-17 (2010)
Kofman R.S., Herd C.D.K., Froese D.G., The Results of the Investigation of the Whitecourt Crater (Alberta, Canada), GeoCanada 2010 – Working with the Earth
Herd, C. D., Froese, D. G., Walton, E. L., Kofman, R. S., Herd, E. P., & Duke, M. J., 2008, Anatomy of a Young Impact Event in Central Alberta: Prospects for the ‘Missing’ Holocene Impact Record: Geology, 36, 955-958.
Herd, C. D., Froese, D. G., Walton, E. L., Kofman, R. S., Herd, E. P., & Duke, M. J., 2008, The Discovery of a Late Holocene Impact Crater Near Whitecourt Alberta: 71st Meeting of the Meteoritical Society, 2008.