Photometry of Jupiter Family Comet nuclei

Photometry of Jupiter Family Comet nuclei

Colin Snodgrass

European Southern Observatory, Chile Alan Fitzsimmons, Stephen Lowry

Queen’s University Belfast, UK

Colin Snodgrass

European Southern Observatory, Chile Alan Fitzsimmons, Stephen Lowry

Queen’s University Belfast, UK

Cometary nucleiCometary nuclei

Nuclei are small (radii a few kilometres) & dark (albedos typically only 4%)

When active, the nucleus is obscured by coma unless imaged at very high spatial resolution.

Nuclei are small (radii a few kilometres) & dark (albedos typically only 4%)

When active, the nucleus is obscured by coma unless imaged at very high spatial resolution.

Observing the nucleusObserving the nucleus

Canonical cut off for activity is Rh = 3 AU. We perform multi-filter, time-series photometry

(CCD imaging). Requires 2-4m class telescope. From this we can measure surface properties

(colours) and the bulk physical parameters of size, shape, rotation period and density.

By studying a large number of comets in this way, we can constrain the general properties of the population.

Canonical cut off for activity is Rh = 3 AU. We perform multi-filter, time-series photometry

(CCD imaging). Requires 2-4m class telescope. From this we can measure surface properties

(colours) and the bulk physical parameters of size, shape, rotation period and density.

By studying a large number of comets in this way, we can constrain the general properties of the population.

Bulk DensitiesBulk Densities

Light-curve amplitude against spin-rate. Minimum bulk density for each minor body (rubble pile). Cut off gives average bulk density for population.

Light-curve amplitude against spin-rate. Minimum bulk density for each minor body (rubble pile). Cut off gives average bulk density for population.

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Bulk Densities (2)Bulk Densities (2)

Same plot for KBOs - split into small (r<200km) and large. KBOs appear to have a similar cut off to JFCs, despite

different sizes of observed bodies.

Same plot for KBOs - split into small (r<200km) and large. KBOs appear to have a similar cut off to JFCs, despite

different sizes of observed bodies.

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Surface ColoursSurface Colours

There is a linear relationship between the measured colour indices (V-R) and (R-I).

This implies increasing albedo through V, R & I bands, i.e. greater reflectance at greater wavelength.

There is a linear relationship between the measured colour indices (V-R) and (R-I).

This implies increasing albedo through V, R & I bands, i.e. greater reflectance at greater wavelength.

Surface Colours (2)Surface Colours (2)

The same relationship between (V-R) and (R-I) holds for KBOs.

Nuclei are found to be red, but not as red as KBOs.

This is attributed to removal or covering of the ‘ultra-red matter’ seen in KBOs by cometary activity.

The same relationship between (V-R) and (R-I) holds for KBOs.

Nuclei are found to be red, but not as red as KBOs.

This is attributed to removal or covering of the ‘ultra-red matter’ seen in KBOs by cometary activity.

Surface Colours (3)Surface Colours (3)

Reducing the colours to a single parameter gives approximately normal distributions for both JFCs and KBOs.

The JFC distribution can be reproduced by applying a linear ‘de-reddening’ function to the KBO one: i.e. the reddest surfaces are the most depleted.

Reducing the colours to a single parameter gives approximately normal distributions for both JFCs and KBOs.

The JFC distribution can be reproduced by applying a linear ‘de-reddening’ function to the KBO one: i.e. the reddest surfaces are the most depleted.

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SummarySummary

We have time-series photometry on a reasonable sample of JFC nuclei.

From this we can constrain the average bulk properties of the population: Spin up/down by jets gives a flat spin rate distribution. A cut off in spin-rate axial-ratio space implies a low average bulk

density of 0.6 g cm-3. This implies considerable porosity.

Density / internal structure similar to KBOs? Colours are less red than KBOs.

Distribution can be recreated from KBO colours.

We have time-series photometry on a reasonable sample of JFC nuclei.

From this we can constrain the average bulk properties of the population: Spin up/down by jets gives a flat spin rate distribution. A cut off in spin-rate axial-ratio space implies a low average bulk

density of 0.6 g cm-3. This implies considerable porosity.

Density / internal structure similar to KBOs? Colours are less red than KBOs.

Distribution can be recreated from KBO colours.