"+specType[nstar]+"),"); Artist's impression of the exoplanet 51 Pegasi b orbiting a star similar to the Sun about 50 light-years away from Earth. The precise amount of time in Earth days it takes for each planet to complete its orbit can be seen below. across the star), the total light output drops accordingly. Of course, this calc is not limited to planets and suns - satellites, moons, comets, asteroids etc. Evidence for a Distant Giant Planet in the Solar System " , by Konstantin Batygin and Michael E. Brown, Division of Geological and Planetary Sciences, California Institute of Technology, The Astronomical Journal, February, 2016 The planet may be too small or the star too far away (and modified by Isaac Newton) or from the Archive for a table query), then it is derived from the stellar effective temperature, Teff , and stellar radius, Simply click on Some exoplanets have been imaged directly by telescopes, but the vast majority have been detected through indirect methods, such as the transit method and the radial-velocity method . Knowing the period of the planet’s orbit around the host star, the inclination of the exoplanet’s orbit with respect to the Earth’s line-of-sight can also be determined. Get orbital period of exoplanet from light curve using astropy.timeseries I am using astropy and I would like to calculate orbital period of an exoplanet by its star's light curve. Learn more about extrasolar planets in this article. and read off its mass. While Kepler's third law was derived from data for planets in A massive exoplanet orbiting in a double star system 336 light-years away may be similar to the alleged "Planet Nine" that may exist on the outskirts of our solar system, according to a new study. The graph plots the un-calibrated signal minus the Orbital period: Add . The fully defined version of Kepler's third law is used to calculate the orbital period of a planet. by the inverse square law: The predicted radial velocity semi-amplitude, K, depends on the planet period, P, planet mass, Mp, the stellar mass, Currently we fix the eccentricity at zero, and an inclination of 90° is assumed for the "Earth-like" and "Jupiter-like" input options. We do not exclude the pulsational nature of the 128-d variations in α Per. Find the distance: Use the average period P in years and It is a particularly advantageous method for space-based observatories that can stare continuously at stars for weeks or months. (Press the calculate button to convert the period of With both mass and size ... days, half the period of the Moon’s orbit around Earth. In a fun cosmic coincidence, researchers used old Kepler spacecraft data to discover an Earth-sized exoplanet with an orbital period of 3.14 days, a … Examples include a change in transit time (known as TTV) of one planet, due to the presence of others in multiple planet systems and pulsar timing, where anomalous movement (measured at radio wavelengths) can be used to infer the presence of a planet. More than 4,000 are known, and about 6,000 await further confirmation. Until very recently, the most common method of exoplanet detection involves radial velocity measurements. the semi-major axis of the planet's orbit about the star This is because the effect of the ‘wobble’ of the star is larger when the difference in mass of the star and the planet is higher. our solar system it has been found to provide _____ method can determine an exoplanet's mass and _____ method can determine an exoplanet's size. Generally, organisms can not survive if water is frozen (0 C = 273 K) or near its boiling point (100 C or 373 K). It is only for transiting exoplanets that astronomers have been able to get direct estimates of the exoplanet mass and radius. The planet mgith be too far away from the star to have I should note that the actual mean temperature of the Earth is ~16 °C. You can calculate the speed of … This is a signal that the period used to calculate the phase was incorrect. The average distance between a planet and its parent star is The inner and outer boundaries are Calculate: a) The distance of the exoplanet from the star b) The exoplanet's orbital speed (Recall 1M, = 1.99 x 1030 kg) Get more help from Chegg The exoplanet is detected by observing a change in periodic phenomena due to the presence of an exoplanet. Front Cover: The Transiting Exoplanet Survey Satellite (TESS) is shown at work in this illustration. the system period and a cursor allows one to measure radial velocity and thus the curve amplitude (the maximum value of radial velocity) on the graph. For the case where a planet is larger than its host, the transit depth is capped at 100%. Wolf 503b is the only exoplanet that large that can be found near the so-called Fulton gap. For one transit, the most frequently detected orbital period is 8.17days in the region with observation of 27 days and 11.25days in the region near the poles. average signal from the instrument. Astronomers have been able to estimate the mass of a star if For objects in the Solar System, this is often referred to as the sidereal period, determined by a 360° revolution of one celestial body around another, e.g. number in the appropriate empty box below. Locate the spectral type for this star If the stellar luminosity, L*, is not provided explicitly as an input (either from user input parameters for a custom stellar signature, or from the Archive for a table query), then it is derived from the stellar effective temperature, Teff , and stellar radius, R*(if available): Richard L. Bowman Auto-correlation methods were applied to the light curve to deduce a rotation period for the star of 8.87 ± 1.12 days. 2 The State of the Field of Exoplanets. With these parameters at hand astronomers are able to set the most fundamental constraints on models which reveal the physical nature of the exoplanet, such as its average density and surface gravity. This database comprises spectroscopic orbital elements measured for planets orbiting their host stars from radial velocity and transit measurements as … days in the formula below. If you know the satellite’s speed and the radius at which it orbits, you can figure out its period. see how much the star appears to move over 6 months compared to more distant objects. By measuring the depth of the dip in brightness and knowing the size of the star, scientists can determine the size or radius of the planet. Period = days (1 yr / 365.25 days) Period = yr (Press the calculate button to convert the period of the exoplanet from days into years.) - The temperature of a planet similar to Jupiter can be approximated by the formula below, where T is the temperature in Kelvin degrees, and R is the The equation is similar to for instruments to detect the effect of the planet's transits. causes the larger observed dips in the graph. the exoplanet from days into years. Both the size of the host star and the planet will determine the decrease in flux during the transit. Then enter this period in Wolf 503b completes one orbit in as few as six days because it is very close to the star. Maybe no planet passes directly in front of this star, can be found in "The Exoplanet Handbook," Perryman, 2011. For the special case of circular orbits, the semimajor axis is equal to the radius. Moving on to the third candidate in the sorted orbital period column then yields the exoplanet HR 8799 b. The study of exoplanets is a relatively new field of astronomy. not support JavaScript. I follow tutorial in astropy docs and I use data from Kepler in Nasa Exoplanet Archive. Some planets discovered by Kepler orbit around their stars so quickly that their years only last about four hours! Period = yr When we plot the points in a phase diagram, we see this: Hey! 5b is the first exoplanet discovered around the fifth star found to have a planet. The shape of a transit light curve gives astronomers a wealth of information about an exoplanet. will definitely match this assumption. If no significant dips in the signal are observable, While news articles in the popular scientific press often refer our Sun as an “ordinary star”, in fact it is somewhat large compared to the general star population – about 70% of stars in our galaxy are red dwarfs, which are stars that have masses between 7.5% and 50%that of our Sun. Its orbital period of 112 days places it in its star’s habitable zone, but with a surface temperature that could be as low as -40°C. They have discovered and examined an exoplanet - TOI-197.01. it is a main sequence star (on the H-R diagram) and if its (2011) documentation can be found below (labeled with '*' in the Summary of Methodology section). At this distance, and with an orbital velocity of 29.78 km/s (18.5 mi/s) the time it take for the planet to complete a single orbit of the Sun (i.e. and should be given in Astronomical Units (AU). Using the demo that simulates an exoplanet transiting in front of its host star, fill in the table below. made a transit during the length of time the instrument was If your browser is displaying this line of text, then it does the … Light Curve of a Planet Transiting Its Star. Kasting, J. F., Whitmire, D. P., & Reynolds, R. T. 1993, Icarus, 101, 108 Determine . This particular Sedna-like exoplanet has a perihelion of 80 AUs and an aphelion of approximately 446 AU and an eccentric orbital period of 4,300 years. " Distance of the Exoplanet from Its Parent Star. star's mass. When the exoplanet passes in front of the star, the light curve will show a dip in brightness. Not all planets have years as long as a year on the Earth! between transits of the planet across the star face. Kasting et al. and David Koch 2 of Cumming et al. The orbital period given for this planet is 164,250 days, or about 450 years (no margin of error is given). The Exoplanet Data Explorer (EDE) gives Web users access to the Exoplanet Orbit Database (EOD). 4. Convert the average period in days to years: 5. Determine the orbital period of this planet in days. We scale these values for stellar luminosity, and neglect any dependency on stellar effective temperature (effectively assuming the planet albedo is constant with wavelength).

defined using the (optimistic) "recent Venus" and "early Mars" models, respectively, from Unsurprisingly the the length of each planet’s year correlates with its distance from the Sun as seen in the graph above. Stellar The transit light curve gives an astronomer a wealth of information about the transiting planet as well as the star. The period of a satellite is the time it takes it to make one full orbit around an object. spectral type is known. star describes an ellipse on the sky whose angular semi-major axis, Δθ, is given by: where the numerical coefficients again reflect the appropriate unit conversions. It also includes some functions generally useful for astronomy, since that's usually the discipline involved in studying exoplanets in the first place. This dimming can be seen in light curves – graphs showing light received over a period of time. The Exoplanet Calcultor includes functions that are useful related to the study of planets outside of our solar-system (exoplanets). In August, MIT researchers identified an exoplanet with an extremely brief orbital period: The team found that Kepler 78b, a small, intensely hot planet 400 light-years from Earth, circles its star in just 8.5 hours — lightning-quick, compared with our own planet’s leisurely 365-day orbit. The first calculation comes from Kepler's Third Law (shown below), where ' G' is Newton's Gravitational Constant.The period, ' P', is the orbital period of the exoplanet, and comes directly from the measured period using, for example, the transit or radial velocity detection methods (Detection Methods page). The period of the Earth as it travels around the sun is one year. Note that this calculation does not include the effect of relativity. The scale of the y-axis renormalizes as needed and the phase of perihelion (closest approach to the star) is assigned a phase of zero. passes in front of the star (making a transit The period of the Earth as it travels around the sun is one year. This is also known as the orbital period. Mercury: 87.97 days (0.2 years) Venus : 224.70 days (0.6 years) The Moon has a period of 27.3 days and has a mean distance of 3.90 105 km from the center of Earth. Calculate the orbital period of the exoplanet and use it to locate the planet's distance from its star; Determine the mass of this newly discovered exoplanet; Procedure. The Exoplanet Orbit Database is a database of well-determined orbital parameters of exoplanets, and their host stars' properties. I usually think about exoplanets about stars similar to the Sun. The period of time while the planet passes in front of the star is called a transit. Note #2: If no transits are observable in the data, then go beack to the The length of time between each transit is the planet's "orbital period", or the length of a year on that particular planet. (Bridgewater College) ... the velocity of the star can be determined and hence we can calculate either a lower limit for the planet's mass or the true mass if the inclination is known. Extrasolar planets were first discovered in 1992. ... measure the size of the orbit and orbital period. The Predicted Observables for Exoplanets (POE) tool calculates habitable zone radii, predicted insolation, and predicted radial velocity, astrometric, and M*, the orbital inclination, i, and the orbital eccentricity, e. We use the following expression to obtain K in ms-1 : where the numerical constants include appropriate unit conversions. When a planet radial velocity, transit. Perryman, M. 2011, The Exoplanet Handbook, Cambridge University Press, New York; ISBN: 0521765595. Documentation and Methodology. One of the exoplanets has a 5.8 day orbital period. But by far, the biggest advantage is that we can determine the atmospheric composition of the exoplanet which is vital in ascertaining its potential for habitability. this with the published value (see exoplanet.eu). If a value for the distance, d, to the system is available, then the radii and width are also calculated in angular units as seen on the sky: The maximum projected separation on the sky of a planet-star pair, for a circular orbit, is a function of the distance to the system, d, and the semi-major axis, a, both in meters. Knowing the period of the planet’s orbit around the host star, the inclination of the exoplanet’s orbit with respect to the Earth’s line-of-sight can also be determined. An outline of the full derivation of the RV semi-amplitude Because red dwarfs are so numerous, some planetary a… The mass of a star is perhaps its most significant feature. Planet Orbital Period (years) Orbital Period (days) Distance from Sun (AU) Distance from Sun (km) Mercury 0.24 years 88.0 days 0.387 AU 57,900,000 km Venus 0.62 years 224.7 days 0.72 AU 108,200,000 km Earth 1 year 365.2 days 1 AU 149,600,000 km may also be input. orbital period) is equal to about 365.25 days. (Find the Masses (in units of solar masses). that the data may be measured more accurately. 1999, but takes the period in days, retains the To determine other properties of the exoplanet such as its mass and thus density, another technique called the Radial Velocity Method is used. R. p, the radius of your exoplanet in kilometers (km) using the lab website and referencing the table below to guide you. The period of a satellite is the time it takes it to make one full orbit around an object. In the Cetus constellation there is a star, HD 1461 (1.078 Ms) that has three confirmed exoplanets. To find the orbital period of an exoplanet using a light curve, determine the length of time between each dip in the light curve, represented by a line that drops below the normal light intensity. that planet is small compared to the mass of its star. why are there more jovian in the exoplanet database. If the stellar luminosity, L*, is not provided explicitly as an input (either from user input parameters for a custom stellar signature, Have students study the light curves provided on the worksheet to determine the orbital period and other properties for Kepler-5b, 6b, 7b and 8b. ), B. The transit observed in this dataset occurs every 3.5250±0.003 days (P) and we can also measure the transit duration (T) and from this the orbital distance (a): If you know the satellite’s speed and the radius at which it orbits, you can figure out its period. The easiest units for mass in this equation are. period P in days semimajor axis a in AU mass Mtot in solar masses then we can determine k very precisely and very simply: just count the days in a year! Then enter this They were awarded the Nobel Prize in physics on October 8th, 2019. The newly discovered exoplanet is a Saturn-like gas planet that orbits around its star with a period of only 14 days. the graph and then print the resulting web page. The third law of planetary motion derived by Johannes Kepler Determine the orbital period of the planet: There are several methods to extract this information from your graph. The Transiting Exoplanet Survey Satellite spotted the planet, as well as a weird "sub-Neptune" world, circling the star HD 21749, which lies about 53 light-years from Earth. Press the "Next Page" button to continue your analysis. It is easier to put these values in terms of the radius of Jupiter (RJ = 71000 km) Now we can calculate the planets orbital distance. From the graph above, calculate the average time Using the precise data from the Kepler exoplanet mission, astronomers from the Harvard-Smithsonian Center for Astrophysics have determined the rotation period measurements for 30 cool stars in the 2.5- billion-year-old stellar cluster NGC 6819.. 3. The predicted transit depth, δ, is given by the ratio of the projected area of the planet to that of the star. The Transiting Exoplanet Survey Satellite spotted the planet, as well as a weird "sub-Neptune" world, circling the star HD 21749, which lies about 53 light-years from Earth. (2002-2011; last updated: 14-Sep-11). exoplanet system is viewed from an interstellar distance so great that the distance to the exoplanet or host star can be considered equal. We define the HZ "center" as 1au for Earth around the Sun, and likewise scale with stellar luminosity: where RHZ represents the various habitable zone radii, and ΔHZ is the habitable zone width. Use at least two different techniques to obtain at least three separate values, then calculate the average period in days. 1993. Essentially all exoplanets discovered to date fit this criteria, (a) Use Kepler's laws to find the period of a satellite in orbit 6.70 103 km from the center of … even if it has one or more planets orbiting it. about its center of mass. Based on data from the NASA Exoplanet Archive: https://exoplanetarchive.ipac.caltech.edu/. Having both the period and the semi-major axis one can estimate the orbital speed (assuming a circular orbit) to be: Determining the radius of an exoplanet. Note #1: If desirable, the plot may be printed so Transit data are rich with information. collecting data. Due to orbital conditions, this very narrow 'zone of life' … The first confirmation of an exoplanet orbiting a main-sequence star was made in 1995, when a giant planet was found in a four-day orbit around the nearby star 51 Pegasi. Conclusions.α Per may have an exoplanet, but the combined data spanning over 20 years seem to suggest that the 128-d RV variations have not been stable on a long-term scale, which is somewhat difficult to reconcile with the exoplanet explanation. Astronomers discover an exoplanet (a planet of a star other than the Sun) that has an orbital period of 3.63 Earth years in its circular orbit around its sun, which is a star with a measured mass of 3.65×1030 kg . Greater displacement of the spectral lines means the exoplanet has a larger mass, therefore an estimate for the planet’s mass can be calculated. Given the stellar luminosity (either explicitly provided, or derived as above), the insolation (power per unit area), S, in Earth units, is given directly day of the first and last transit and divide by the number of The exoplanet is detected by observing a change in periodic phenomena due to the presence of an exoplanet. Astronomers have confirmed the existence of the exoplanet b Pictoris c located in another star system some 63 light years away from Earth - and have shared a picture to prove it. Exoplanet HD 149026b orbits a G type star that has a mass 1.35 times the mass of the Sun, and has a semi-major axis of 0.04 AU. You can check this calculation by setting the masses to 1 Sun and 1 Earth, and the distance to 1 astronomical unit (AU), which is the distance between the Earth and the Sun. See the table. Although it was not the first detected exoplanet (see Box 2.1), the discovery of a planetary companion to the near solar analogue 51 Pegasi by Mayor and Queloz in 1995 launched the field of exoplanets.The discovery of 51 Peg b, which has a minimum mass of roughly 0.5 times the mass of Jupiter (M J) but an orbital period of only about 4 days, surprised many. The first confirmed exoplanet discovery was in 1992, with the discovery of PSR B1257+12 around a pulsar star; the first main-sequence star discovery (51 Pegasi b) was found in 1995. GJ 1132b, also known as Gliese 1132b, circles its host star every 1.6 days at a distance of 1.4 million miles. M Sun. The astrometric amplitude of the wobble of a host star induced by its companion in au is derived straightforwardly from balance of the star/planet system use a browser than supports JavaScript. The transit method is particularly useful for calculating the radius of an exoplanet. document.write("("+specType[nstar]+"),"); Artist's impression of the exoplanet 51 Pegasi b orbiting a star similar to the Sun about 50 light-years away from Earth. The precise amount of time in Earth days it takes for each planet to complete its orbit can be seen below. across the star), the total light output drops accordingly. Of course, this calc is not limited to planets and suns - satellites, moons, comets, asteroids etc. Evidence for a Distant Giant Planet in the Solar System " , by Konstantin Batygin and Michael E. Brown, Division of Geological and Planetary Sciences, California Institute of Technology, The Astronomical Journal, February, 2016 The planet may be too small or the star too far away (and modified by Isaac Newton) or from the Archive for a table query), then it is derived from the stellar effective temperature, Teff , and stellar radius, Simply click on Some exoplanets have been imaged directly by telescopes, but the vast majority have been detected through indirect methods, such as the transit method and the radial-velocity method . Knowing the period of the planet’s orbit around the host star, the inclination of the exoplanet’s orbit with respect to the Earth’s line-of-sight can also be determined. Get orbital period of exoplanet from light curve using astropy.timeseries I am using astropy and I would like to calculate orbital period of an exoplanet by its star's light curve. Learn more about extrasolar planets in this article. and read off its mass. While Kepler's third law was derived from data for planets in A massive exoplanet orbiting in a double star system 336 light-years away may be similar to the alleged "Planet Nine" that may exist on the outskirts of our solar system, according to a new study. The graph plots the un-calibrated signal minus the Orbital period: Add . The fully defined version of Kepler's third law is used to calculate the orbital period of a planet. by the inverse square law: The predicted radial velocity semi-amplitude, K, depends on the planet period, P, planet mass, Mp, the stellar mass, Currently we fix the eccentricity at zero, and an inclination of 90° is assumed for the "Earth-like" and "Jupiter-like" input options. We do not exclude the pulsational nature of the 128-d variations in α Per. Find the distance: Use the average period P in years and It is a particularly advantageous method for space-based observatories that can stare continuously at stars for weeks or months. (Press the calculate button to convert the period of With both mass and size ... days, half the period of the Moon’s orbit around Earth. In a fun cosmic coincidence, researchers used old Kepler spacecraft data to discover an Earth-sized exoplanet with an orbital period of 3.14 days, a … Examples include a change in transit time (known as TTV) of one planet, due to the presence of others in multiple planet systems and pulsar timing, where anomalous movement (measured at radio wavelengths) can be used to infer the presence of a planet. More than 4,000 are known, and about 6,000 await further confirmation. Until very recently, the most common method of exoplanet detection involves radial velocity measurements. the semi-major axis of the planet's orbit about the star This is because the effect of the ‘wobble’ of the star is larger when the difference in mass of the star and the planet is higher. our solar system it has been found to provide _____ method can determine an exoplanet's mass and _____ method can determine an exoplanet's size. Generally, organisms can not survive if water is frozen (0 C = 273 K) or near its boiling point (100 C or 373 K). It is only for transiting exoplanets that astronomers have been able to get direct estimates of the exoplanet mass and radius. The planet mgith be too far away from the star to have I should note that the actual mean temperature of the Earth is ~16 °C. You can calculate the speed of … This is a signal that the period used to calculate the phase was incorrect. The average distance between a planet and its parent star is The inner and outer boundaries are Calculate: a) The distance of the exoplanet from the star b) The exoplanet's orbital speed (Recall 1M, = 1.99 x 1030 kg) Get more help from Chegg The exoplanet is detected by observing a change in periodic phenomena due to the presence of an exoplanet. Front Cover: The Transiting Exoplanet Survey Satellite (TESS) is shown at work in this illustration. the system period and a cursor allows one to measure radial velocity and thus the curve amplitude (the maximum value of radial velocity) on the graph. For the case where a planet is larger than its host, the transit depth is capped at 100%. Wolf 503b is the only exoplanet that large that can be found near the so-called Fulton gap. For one transit, the most frequently detected orbital period is 8.17days in the region with observation of 27 days and 11.25days in the region near the poles. average signal from the instrument. Astronomers have been able to estimate the mass of a star if For objects in the Solar System, this is often referred to as the sidereal period, determined by a 360° revolution of one celestial body around another, e.g. number in the appropriate empty box below. Locate the spectral type for this star If the stellar luminosity, L*, is not provided explicitly as an input (either from user input parameters for a custom stellar signature, or from the Archive for a table query), then it is derived from the stellar effective temperature, Teff , and stellar radius, R*(if available): Richard L. Bowman Auto-correlation methods were applied to the light curve to deduce a rotation period for the star of 8.87 ± 1.12 days. 2 The State of the Field of Exoplanets. With these parameters at hand astronomers are able to set the most fundamental constraints on models which reveal the physical nature of the exoplanet, such as its average density and surface gravity. This database comprises spectroscopic orbital elements measured for planets orbiting their host stars from radial velocity and transit measurements as … days in the formula below. If you know the satellite’s speed and the radius at which it orbits, you can figure out its period. see how much the star appears to move over 6 months compared to more distant objects. By measuring the depth of the dip in brightness and knowing the size of the star, scientists can determine the size or radius of the planet. Period = days (1 yr / 365.25 days) Period = yr (Press the calculate button to convert the period of the exoplanet from days into years.) - The temperature of a planet similar to Jupiter can be approximated by the formula below, where T is the temperature in Kelvin degrees, and R is the The equation is similar to for instruments to detect the effect of the planet's transits. causes the larger observed dips in the graph. the exoplanet from days into years. Both the size of the host star and the planet will determine the decrease in flux during the transit. Then enter this period in Wolf 503b completes one orbit in as few as six days because it is very close to the star. Maybe no planet passes directly in front of this star, can be found in "The Exoplanet Handbook," Perryman, 2011. For the special case of circular orbits, the semimajor axis is equal to the radius. Moving on to the third candidate in the sorted orbital period column then yields the exoplanet HR 8799 b. The study of exoplanets is a relatively new field of astronomy. not support JavaScript. I follow tutorial in astropy docs and I use data from Kepler in Nasa Exoplanet Archive. Some planets discovered by Kepler orbit around their stars so quickly that their years only last about four hours! Period = yr When we plot the points in a phase diagram, we see this: Hey! 5b is the first exoplanet discovered around the fifth star found to have a planet. The shape of a transit light curve gives astronomers a wealth of information about an exoplanet. will definitely match this assumption. If no significant dips in the signal are observable, While news articles in the popular scientific press often refer our Sun as an “ordinary star”, in fact it is somewhat large compared to the general star population – about 70% of stars in our galaxy are red dwarfs, which are stars that have masses between 7.5% and 50%that of our Sun. Its orbital period of 112 days places it in its star’s habitable zone, but with a surface temperature that could be as low as -40°C. They have discovered and examined an exoplanet - TOI-197.01. it is a main sequence star (on the H-R diagram) and if its (2011) documentation can be found below (labeled with '*' in the Summary of Methodology section). At this distance, and with an orbital velocity of 29.78 km/s (18.5 mi/s) the time it take for the planet to complete a single orbit of the Sun (i.e. and should be given in Astronomical Units (AU). Using the demo that simulates an exoplanet transiting in front of its host star, fill in the table below. made a transit during the length of time the instrument was If your browser is displaying this line of text, then it does the … Light Curve of a Planet Transiting Its Star. Kasting, J. F., Whitmire, D. P., & Reynolds, R. T. 1993, Icarus, 101, 108 Determine . This particular Sedna-like exoplanet has a perihelion of 80 AUs and an aphelion of approximately 446 AU and an eccentric orbital period of 4,300 years. " Distance of the Exoplanet from Its Parent Star. star's mass. When the exoplanet passes in front of the star, the light curve will show a dip in brightness. Not all planets have years as long as a year on the Earth! between transits of the planet across the star face. Kasting et al. and David Koch 2 of Cumming et al. The orbital period given for this planet is 164,250 days, or about 450 years (no margin of error is given). The Exoplanet Data Explorer (EDE) gives Web users access to the Exoplanet Orbit Database (EOD). 4. Convert the average period in days to years: 5. Determine the orbital period of this planet in days. We scale these values for stellar luminosity, and neglect any dependency on stellar effective temperature (effectively assuming the planet albedo is constant with wavelength).