Nothing
vismeteor
In vismeteor: Analysis of Visual Meteor Data
knitr::opts_chunk$set(
collapse = TRUE,
comment = "#>"
)
library(vismeteor)
knitr::opts_chunk$set(
collapse = TRUE,
comment = "#>"
)
Introduction
vismeteor was developed to provide a comprehensive tool for analyzing visually observed
meteors. It takes into account human perception of different meteor magnitudes through
perception probabilities. Therefore, this package provides methods that incorporate
these perception probabilities in the evaluation of meteor magnitudes.
Perception probabilities are crucial for analyzing observed magnitude distributions,
as they give rise to specific distributions unique to visual meteor observations.
One such model is the Geometric Model of Visual Meteor Magnitudes.
It is based on the standard geometric distribution, adjusted by multiplying its probabilities with
the perception probabilities. The resulting distribution has a single parameter:
the population index r.
This package provides functions to work with this adjusted distribution.
Additionally, this package offers tools to facilitate the evaluation, recognizing that
visual meteor observations typically report only total counts over a specified period,
rather than individual meteor events.
For visual observations of meteor magnitudes, the observed counts can be specified in
fractional values (half meteors). This package includes a function for unbiased rounding
of these fractional values to use standard tools in R that only allow integer values.
Perception probabilities
Meteors appear randomly distributed across the sky. The perception of an observer can
vary significantly for each meteor, influenced largely by the region of the sky where
the meteor appears. Depending on its position, a meteor might be perceived or missed entirely,
leading to the concept of perception probabilities.
Perception probabilities quantify the likelihood of an observer detecting a meteor.
They provide a statistical measure reflecting the chance of seeing or not seeing a meteor
under various conditions. In statistical modeling of visual observations, these probabilities
are commonly expressed in relation to the difference between the meteor's magnitude and the
limiting magnitude of the observation.
This package includes the function vmperception() to return perception probabilities for
visual meteor magnitudes. For advanced analytical purposes, vmperception.l() is provided
to return the Laplace-transformed perception probabilities.
Custom perception probability functions can be passed to most functions of this package.
This allows users to tailor the behavior of the functions to their specific needs and
conduct their own studies on the appearance of observable meteor magnitudes.
This flexibility is particularly valuable for researchers wishing to incorporate
their own empirical data or models into the analysis.
See ?vmperception and ?vmperception.l for more information.
Geometric Model of Visual Meteor Magnitudes
In visual meteor observations, magnitudes are typically recorded as integer values.
Hence, the geometric model is discrete and its probability mass function is
$$
{\displaystyle P[X = x] \sim f(x) \, \mathrm r^{-x}} \,\mathrm{,}
$$
where $x \ge -0.5$ denotes the difference between the limiting magnitude and the
meteor magnitude, and $f(x)$ is the perception probability function.
This distribution is the product of the perception probabilities and the
underlying geometric distribution of meteor magnitudes.
Therefore, the parameter $p$ of the geometric distribution is $p = 1 - 1/r$.
The main advantage of this model is its simplicity.
When the number of observed meteors is small, it can often be shown that the
distribution of meteor magnitudes is well described by this model.
m <- seq(6, -4, -1)
limmag <- 6.5
r <- 2.0
p <- vismeteor::dvmgeom(m, limmag, r)
barplot(
p,
names.arg = m,
main = paste0('Density (r = ', r, ', limmag = ', limmag, ')'),
col = "blue",
xlab = 'm',
ylab = 'p',
border = "blue",
space = 0.5
)
axis(side = 2, at = pretty(p))
See ?vmgeom for more information.
Ideal Distribution of Meteor Magnitudes
The ideal model of visual meteor magnitudes is an alternative to the geometric model.
It more accurately accounts for the finiteness of meteor magnitudes across the entire
magnitude spectrum, using the ideal gas from theoretical physics as a conceptual analogy.
This model is particularly useful when, compared to the geometric model,
fewer faint meteor magnitudes are observed.
The density of the ideal distribution is
$$
{\displaystyle \frac{\mathrm{d}p}{\mathrm{d}m} = \frac{3}{2} \, \log(r) \sqrt{\frac{r^{3 \, \psi + 2 \, m}}{(r^\psi + r^m)^5}}}
$$
where $m$ is the meteor magnitude, $r = 10^{0.4} \approx 2.51189 \dots$ is a constant and
$\psi$ is the only parameter of this magnitude distribution.
m <- seq(6, -4, -1)
psi <- 5.0
limmag <- 6.5
p <- vismeteor::dvmideal(m, limmag, psi)
barplot(
p,
names.arg = m,
main = paste0('Density (psi = ', psi, ', limmag = ', limmag, ')'),
col = "blue",
xlab = 'm',
ylab = 'p',
border = "blue",
space = 0.5
)
axis(side = 2, at = pretty(p))
See ?mideal and ?vmideal for more information.
Fractional Counting
In the statistical analysis of visual meteor observations, a method known as "count data"
in categorical time series is used. Observers record the number of meteors in each category
over specific time intervals.
In visual meteor observation, observers record numerical meteor magnitudes and sum them,
uniquely allowing for "half" counts when indecisive between two values. This fractional
counting reflects measurement uncertainty, splitting counts between adjacent magnitude categories.
While fractional counting accommodates measurement uncertainty with "half" counts, some tools
cannot process these fractional values and require integer rounding.
The function vmtable() addresses this by rounding the magnitudes in a contingency table to whole
numbers. It ensures that the rounding process only alters the marginal totals when necessary,
preserving the overall count integrity. This means both the grand total and the intermediate
sums of meteors observed remain consistent, ensuring accurate and usable data for
subsequent analysis.
Example:
mt <- as.table(matrix(
c(
0.0, 0.0, 2.5, 0.5, 0.0, 1.0,
0.0, 1.5, 2.0, 0.5, 0.0, 0.0,
1.0, 0.0, 0.0, 3.0, 2.5, 0.5
), nrow = 3, ncol = 6, byrow = TRUE
))
colnames(mt) <- seq(6)
rownames(mt) <- c('A', 'B', 'C')
margin.table(mt, 1)
margin.table(mt, 2)
# contingency table with integer values
(mt.int <- vmtable(mt))
margin.table(mt.int, 1)
margin.table(mt.int, 2)
See ?vmtable for more information.
Quantile Analysis with Minimum Meteor Count
The function freq.quantile() is tailored for analyzing time series data in visual
meteor observation, where the count of meteors is recorded over specific time intervals.
Unlike traditional methods that sort quantiles based on time and percent, which often result
in some quantiles having fewer meteors than desired, freq.quantile() constructs quantiles
with a focus on ensuring a minimum number of meteors in each quantile.
This method addresses the challenge of varying meteor counts in each interval, including those
with zero meteors. By utilizing freq.quantile(), users can effectively divide the time series
into quantiles that are both time-based and density-based, enhancing the understanding of meteor
occurrence and distribution over the observed period while ensuring each quantile meets the
minimum count criterion.
This approach provides a more nuanced and reliable analysis, especially vital when dealing with
the inherent variability in meteor observations.
The following example represents a time-ordered list of observed meteor counts.
The objective is to group these counts into quantiles while maintaining their chronological order,
ensuring that each quantile contains at least 10 meteors.
freq <- c(1,8,3,3,4,9,5,0,0,2,7,8,2,6,4)
f <- freq.quantile(freq, 10)
print(f)
print(tapply(freq, f, sum))
See ?freq.quantile for more information.
Interfacing VMDB Data with load_vmdb()
The load_vmdb() function is designed to interface with the
imo-vmdb
application, processing data specifically exported from the Visual Meteor Database (VMDB) in
CSV format. After these CSV exports are verified and validated with the imo-vmdb application,
they are stored in a relational database, which enhances the accessibility and usability of the
data compared to its original CSV format. This storage method establishes relationships between
data records and enriches them with additional information derived from the original data records.
Utilizing load_vmdb(), users can efficiently query and retrieve specific datasets relevant
to their meteor observation analysis. This streamlined access facilitates more comprehensive
and targeted research.
Within this package, PER_2015_rates and PER_2015_magn are provided as example data sets.
They are included for testing and training purposes, allowing users to
understand and utilize the full functionality of the entire package.
See ?load_vmdb, ?PER_2015_rates and ?PER_2015_magn for more information.
Try the vismeteor package in your browser
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vismeteor documentation built on Sept. 9, 2025, 5:38 p.m.
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knitr::opts_chunk$set( collapse = TRUE, comment = "#>" )
library(vismeteor) knitr::opts_chunk$set( collapse = TRUE, comment = "#>" )
Introduction
vismeteor was developed to provide a comprehensive tool for analyzing visually observed
meteors. It takes into account human perception of different meteor magnitudes through
perception probabilities. Therefore, this package provides methods that incorporate
these perception probabilities in the evaluation of meteor magnitudes.
Perception probabilities are crucial for analyzing observed magnitude distributions, as they give rise to specific distributions unique to visual meteor observations. One such model is the Geometric Model of Visual Meteor Magnitudes. It is based on the standard geometric distribution, adjusted by multiplying its probabilities with the perception probabilities. The resulting distribution has a single parameter: the population index r. This package provides functions to work with this adjusted distribution.
Additionally, this package offers tools to facilitate the evaluation, recognizing that visual meteor observations typically report only total counts over a specified period, rather than individual meteor events.
For visual observations of meteor magnitudes, the observed counts can be specified in fractional values (half meteors). This package includes a function for unbiased rounding of these fractional values to use standard tools in R that only allow integer values.
Perception probabilities
Meteors appear randomly distributed across the sky. The perception of an observer can vary significantly for each meteor, influenced largely by the region of the sky where the meteor appears. Depending on its position, a meteor might be perceived or missed entirely, leading to the concept of perception probabilities.
Perception probabilities quantify the likelihood of an observer detecting a meteor. They provide a statistical measure reflecting the chance of seeing or not seeing a meteor under various conditions. In statistical modeling of visual observations, these probabilities are commonly expressed in relation to the difference between the meteor's magnitude and the limiting magnitude of the observation.
This package includes the function vmperception() to return perception probabilities for
visual meteor magnitudes. For advanced analytical purposes, vmperception.l() is provided
to return the Laplace-transformed perception probabilities.
Custom perception probability functions can be passed to most functions of this package. This allows users to tailor the behavior of the functions to their specific needs and conduct their own studies on the appearance of observable meteor magnitudes. This flexibility is particularly valuable for researchers wishing to incorporate their own empirical data or models into the analysis.
See ?vmperception and ?vmperception.l for more information.
Geometric Model of Visual Meteor Magnitudes
In visual meteor observations, magnitudes are typically recorded as integer values.
Hence, the geometric model is discrete and its probability mass function is
$$
{\displaystyle P[X = x] \sim f(x) \, \mathrm r^{-x}} \,\mathrm{,}
$$
where $x \ge -0.5$ denotes the difference between the limiting magnitude and the
meteor magnitude, and $f(x)$ is the perception probability function.
This distribution is the product of the perception probabilities and the
underlying geometric distribution of meteor magnitudes.
Therefore, the parameter $p$ of the geometric distribution is $p = 1 - 1/r$.
The main advantage of this model is its simplicity.
When the number of observed meteors is small, it can often be shown that the
distribution of meteor magnitudes is well described by this model.
m <- seq(6, -4, -1) limmag <- 6.5 r <- 2.0 p <- vismeteor::dvmgeom(m, limmag, r) barplot( p, names.arg = m, main = paste0('Density (r = ', r, ', limmag = ', limmag, ')'), col = "blue", xlab = 'm', ylab = 'p', border = "blue", space = 0.5 ) axis(side = 2, at = pretty(p))
See ?vmgeom for more information.
Ideal Distribution of Meteor Magnitudes
The ideal model of visual meteor magnitudes is an alternative to the geometric model. It more accurately accounts for the finiteness of meteor magnitudes across the entire magnitude spectrum, using the ideal gas from theoretical physics as a conceptual analogy.
This model is particularly useful when, compared to the geometric model, fewer faint meteor magnitudes are observed.
The density of the ideal distribution is
$$ {\displaystyle \frac{\mathrm{d}p}{\mathrm{d}m} = \frac{3}{2} \, \log(r) \sqrt{\frac{r^{3 \, \psi + 2 \, m}}{(r^\psi + r^m)^5}}} $$ where $m$ is the meteor magnitude, $r = 10^{0.4} \approx 2.51189 \dots$ is a constant and $\psi$ is the only parameter of this magnitude distribution.
m <- seq(6, -4, -1) psi <- 5.0 limmag <- 6.5 p <- vismeteor::dvmideal(m, limmag, psi) barplot( p, names.arg = m, main = paste0('Density (psi = ', psi, ', limmag = ', limmag, ')'), col = "blue", xlab = 'm', ylab = 'p', border = "blue", space = 0.5 ) axis(side = 2, at = pretty(p))
See ?mideal and ?vmideal for more information.
Fractional Counting
In the statistical analysis of visual meteor observations, a method known as "count data" in categorical time series is used. Observers record the number of meteors in each category over specific time intervals.
In visual meteor observation, observers record numerical meteor magnitudes and sum them, uniquely allowing for "half" counts when indecisive between two values. This fractional counting reflects measurement uncertainty, splitting counts between adjacent magnitude categories.
While fractional counting accommodates measurement uncertainty with "half" counts, some tools
cannot process these fractional values and require integer rounding.
The function vmtable() addresses this by rounding the magnitudes in a contingency table to whole
numbers. It ensures that the rounding process only alters the marginal totals when necessary,
preserving the overall count integrity. This means both the grand total and the intermediate
sums of meteors observed remain consistent, ensuring accurate and usable data for
subsequent analysis.
Example:
mt <- as.table(matrix( c( 0.0, 0.0, 2.5, 0.5, 0.0, 1.0, 0.0, 1.5, 2.0, 0.5, 0.0, 0.0, 1.0, 0.0, 0.0, 3.0, 2.5, 0.5 ), nrow = 3, ncol = 6, byrow = TRUE )) colnames(mt) <- seq(6) rownames(mt) <- c('A', 'B', 'C') margin.table(mt, 1) margin.table(mt, 2) # contingency table with integer values (mt.int <- vmtable(mt)) margin.table(mt.int, 1) margin.table(mt.int, 2)
See ?vmtable for more information.
Quantile Analysis with Minimum Meteor Count
The function freq.quantile() is tailored for analyzing time series data in visual
meteor observation, where the count of meteors is recorded over specific time intervals.
Unlike traditional methods that sort quantiles based on time and percent, which often result
in some quantiles having fewer meteors than desired, freq.quantile() constructs quantiles
with a focus on ensuring a minimum number of meteors in each quantile.
This method addresses the challenge of varying meteor counts in each interval, including those
with zero meteors. By utilizing freq.quantile(), users can effectively divide the time series
into quantiles that are both time-based and density-based, enhancing the understanding of meteor
occurrence and distribution over the observed period while ensuring each quantile meets the
minimum count criterion.
This approach provides a more nuanced and reliable analysis, especially vital when dealing with the inherent variability in meteor observations.
The following example represents a time-ordered list of observed meteor counts. The objective is to group these counts into quantiles while maintaining their chronological order, ensuring that each quantile contains at least 10 meteors.
freq <- c(1,8,3,3,4,9,5,0,0,2,7,8,2,6,4) f <- freq.quantile(freq, 10) print(f) print(tapply(freq, f, sum))
See ?freq.quantile for more information.
Interfacing VMDB Data with load_vmdb()
The load_vmdb() function is designed to interface with the
imo-vmdb
application, processing data specifically exported from the Visual Meteor Database (VMDB) in
CSV format. After these CSV exports are verified and validated with the imo-vmdb application,
they are stored in a relational database, which enhances the accessibility and usability of the
data compared to its original CSV format. This storage method establishes relationships between
data records and enriches them with additional information derived from the original data records.
Utilizing load_vmdb(), users can efficiently query and retrieve specific datasets relevant
to their meteor observation analysis. This streamlined access facilitates more comprehensive
and targeted research.
Within this package, PER_2015_rates and PER_2015_magn are provided as example data sets.
They are included for testing and training purposes, allowing users to
understand and utilize the full functionality of the entire package.
See ?load_vmdb, ?PER_2015_rates and ?PER_2015_magn for more information.
Try the vismeteor package in your browser
Any scripts or data that you put into this service are public.
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