Leon Stilwell. Bow Shocks in Exoplanets. By: Leon Stilwell

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1 Bow Shocks in Exoplanets By: Leon Stilwell 1

2 Abstract: Bow shocks are a fascinating component of our universe. These little known phenomena have been postulated to be a reason life has developed on Earth. These structures occur when the planet s magnetic field comes into contact with the radiation emitted from the star. In this study, we observed several exoplanets using a method described by Vidotto et al (2010) which involved taking measurements in the UV and IR wavelengths. These were then plotted into light curves and examined for differences. Unfortunately, the anticipated results were not detected. Instead, we ended up with non-detections. This should not discourage further observations, especially because one of the data sets appeared flawed. 2

3 Introduction Long before the first confirmed exoplanet detection about twenty years ago (Wolszczan and Frail, 1992), humans have been fascinated with the possibility of life on planets outside our solar system and have pursued the search for exoplanets systematically. Exoplanets, which are simply planets found in other star systems, have long held the interest of scientists in the search for habitable worlds. At the time of this writing, out of the 1038 exoplanets discovered, 387 have been found to be transiting (Zolotukhin, 1995), with more detections happening almost every day. Swift et al. predicts that there are at least one hundred billion planets in our galaxy alone, which averages out to about one planet per star (2012). Life of course is possible outside of Earth, but it requires a very specific set of parameters to be within a certain range. Once we discover a planet, we can determine if it exhibits these certain parameters. For example, the planet must lie within a certain distance from its host star in an area known as the habitable zone, an area where water can be found in the liquid state on the surface. As restrictive as this may seem, odds are on our side. Currently, about 100 exoplanets have been discovered using the optical transit method alone (Vidotto, Jardine, and Helling 2011). Characteristics such as planet radius, orbital period, and stellar mass can and have been determined using the optical transit method (Seager, & Mallen-Ornelas, 2003). Optical transits can be obtained by observing the target star in the visible spectrum of light. If there is a decrease in the light output of a star as over an interval of time on a consistent basis, it is safe to assume it is due to a planet orbiting the 3

4 star. However, other aspects of a planet could be determined by observing the strength of the light emitted in different wavelengths by the host star, and how they change as the exoplanet orbits. The existence of a bow shock surrounding a transiting exoplanet could be found by obtaining the UV and IR emission from its host star. Bow shock is a term used to describe the interaction between a planet s magnetic field and the stellar wind of its parent star. Once the relative motion between these two fields reaches supersonic speeds, a bow shock is formed (Vidotto et al., 2011). The presence of a bow shock is believed to be vital to life on a planet because a bow shock is able to deflect the solar wind of the parent star. Solar winds can travel at speeds of up between 400 and 800 km s -1 and are potentially dangerous to life forms on the surface of the planet (Vidotto, 2013). Detecting and confirming a bow shock could allow us to determine the diameter of the magnetic field of a planet. This phenomenon can be detected by measuring the difference between the UV emission strength and the infrared emission strength. Taking into account the velocity of the planet, we can determine the stand-off distance, or the distance from the surface of the planet to its magnetic field. Detecting bow shocks in exoplanets requires us to make use of the ultraviolet wavelength and the infrared wavelength. If a bow shock exists, it will absorb some of the ultraviolet light coming from the parent star. This would result in stronger readings in the infrared than in the ultraviolet. 4

5 Vidotto et. al suggest that if there is a bow shock present, it s shocked material will absorb stellar radiation and an early ingress in the UV light curve of the transiting planet will be observed. No early egress will be observed because the shock is only present ahead of the planet s orbit. In addition to postulating this theory, Vidotto put forward several likely planets to harbor bow shocks, including TReS-3b and CoRoT-2b, among others (2010). Furthermore, since the bow shock and magnetic field of our own planet is not completely understood, learning about other planet s bow shocks could help us learn more about our own planet by providing us with a larger sample size to work with as well as providing us with information about the exoplanet we are looking at. In addition to providing clues as to the habitability of an exoplanet, learning about another planet s bow shocks could help us learn more about our own planet by providing us with a larger sample size to compare to the characteristics of our own planet Earth, since the bow shock and magnetic field of our own planet are not completely understood. However, as of today, there is little data on the bow shocks of exoplanets. In this study, we created light curves from transiting exoplanets that show a difference between their infrared and ultraviolet light curves. If detected, we would have more planets that would be considered prime candidates to for a habitable surface that would allow life to exist. As suggested by Vidotto (2010), light curves of WASP-18b were examined for signs of an early ingress, which would indicate the presence of a bow shock. 5

6 The goal of this study is to determine if ground based observations of planetary transits in the UV and near IR wavelengths are sufficient enough to find a bow shocks and analyze the magnetic fields of planets. Materials and Methods All of the observations taken for this project were conducted at the Mauna Kea Observatory, located on the summit of Mauna Kea, Hawaii, USA. Both the Bessel B ( nm) filter and the SDSS-I (748.1 nm) filter were used. The Bessel-B filter records the ultraviolet (UV) wavelength while the SDSS-I filter records the Near-Infrared (Near-IR) wavelength. In order for the data collection to be meaningful, it was necessary to observe the target during a transit. Jeff Coughlin s Extrasolar Planet Transit Finder was useful for this aspect (Coughlin, J. L.). Due to the telescope s physical distance, it was necessary to perform some steps through a proxy. An observation plan was sent to a scientist on site in Hawaii who would then program the observations into the telescope and relay the data back through . The data, obtained in FITS format, was then opened with the program MaxIM DL ( Using the photometry tool inside of the MaxIm DL program, the magnitude of the target star and a reference star were extracted from each image, from both the UV set and then the Near-IR set. The reference star is chose to correct for the natural twinkling or variation in the light recorded by our instruments on the ground due to subtle variations from the atmosphere directing more or less light into the telescope. 6

7 Since the stars all twinkle at the same rate, using other stars from the same portion of the sky allows us to correct that twinkle. For example, if the target star gets 10% brighter due to twinkling, both the check star and the reference star will get 10% brighter as well. This means that the stars all appear 1.1 times as bright as they actually are. The actual brightness of the target star can be determined using the equation,. The values for the brightness of the target star was plotted over time, using Julian Dates, as its planet transited. As suggested by Vidotto (2010), if there is a bow shock present, we should observe an early transit ingress in the light curve of the transiting exoplanet. The shocked material of the bow shock would absorb stellar radiation and an early ingress would be observed. According to Vidotto, no early egress would be observed because the shock is only present ahead of the planet s orbit, not behind it. In addition to postulating this theory, Vidotto (2010) put forward several likely planets to harbor bow shocks, including TReS-3b and CoRoT-2b, among many others. Results studied. The following results will be comprised of three separate sections, one for each planet 7

8 HAT-p-7b We find that there is little variation between light curves in the UV and the IR spectra. As you can see below, as the observation went on over time, the measurements in both the UV and the IR remained fairly constant Magnitude HAT-p-7: Magnitude over time UV Target IR target JD 8

9 WASP-18b For WASP-18b, we discovered a result similar to HAT-p-7b. Once again, we found no discernible difference in the light curves of the UV and the IR. In fact, they appear remarkably similar. WASP-18b: magnitude over time H UV Target IR Target 9

10 HAT-p-32 The last planet studied was HAT-p-32. This data is difficult to read and hard to draw any conclusions from. It might be safe to say that this data is flawed and there was an error in the collection of this set HAT-p-32: Magnitude over Time IR Target UV Target Discussion This study was conducted in order to attempt to detect bow shocks on several exoplanets. Using the method proposed by Vidotto et al (2010), we expected to find some. Unfortunately, the results do not agree with the hypothesis posed. As we can see from the light 10

11 curves, there was no observable difference between the UV and IR spectra in any of the three data sets, signaling non-detections in each. The data received from HAT-p-32 was unexpectedly found to be almost entirely unusable. This is unfortunate as during this project I was under severe time constraints. Given more time, another set of observations could easily be taken of the same target. In fact, more observations of each target could be taken to ensure accuracy of the data collected over the course of this study. Despite these non-detections of a bow shock in two of the targets, as well as an observational error in one; these results, although disappointing, should not discourage further research or observations on bow shocks, as there is always the possibility that further observations and research might yield different results. Fortunately, these results are by no means definitive and hopefully these results could be attributed to observational errors and could be reproduced with greater success at a later point in time with another set of observations. As far as I am aware, this was one of the first studies to focus on bow shocks in exoplanets. However, this project had a very limited scope. Ideally, this process could be repeated for each and every transiting exoplanet to search for bow shocks. A more realistic, time efficient option would be to focus on exoplanets that that are likely to contain the bow shocks, as discussed in detail by Vidotto et al (2010). 11

12 Conclusion In this study, we attempted to detect bow shocks on several exoplanets. However, no bow shocks could found using these sets of observations. However, more observations, on other planets, or even the ones I studied, need to be done using this method to verify its accuracy and potential as a legitimate method to find bow shocks. More work could be done to develop alternate methods in the case that this method is ineffective. Furthermore, we must perform more research on bow shocks to determine their frequency throughout the universe. Even though bow shocks do not directly tell us if life is present on another planet, it takes us one step closer to reaching that goal. In addition, if additional bow shocks could be found in other planetary systems, we could further study the magnetic fields of exoplanets, and perhaps use this information to find even more. Special Thanks I would like to thank both of my science research teachers, Ms. Kleinman and Ms. Foisy for all of their help and support throughout the years. I would also like to thank my mentor Dr. JD Armstrong from the University of Hawaii for his help with this project over the past three years. In addition, I would like to thank Dr. Frits Paerels from Columbia University for his time, invaluable help and generosity towards the end of this project. 12

13 Wolsczan, A., & Frail, D. A. (1992). A planetary system around the millisecond pulsar psr Nature, Vidotto, A., Jardine, M., & Helling, C. (2011). Transit variability in bow shock-hosting planets.. Monthly Notices of the Royal Astronomical Society,414(2), doi: /j x Seager, S., & Mallén-Ornelas, G. (2003). A unique solution of planet and star parameters from an extrasolar planet transit light curve. Astrophysical Journal,585, doi: / Swift, J. J., J.A., J., Morton, T. D., Crepp, J. R., Montet, B. T., Fabrycky, D. C., & Muirhead, P. S. (2012). Characterizing the cool kois iv: Kepler-32 as a prototype for the formation of compact planetary systems throughout the galaxy. Astrophysical Journal, Léger, A. (2000). Strategies for remote detection of life darwin-irsi and tpf missions. Advances in Space REsearch, 25(11), doi: /S (99) Vidotto, A. A., Jardine, M., & Helling, C. (2010). Early uv ingress in wasp-12b: Measuring planetary magnetic fields. The Astrophysical Journal, 168-, Vidotto, A. A., Jardine, M., & Helling, C. (2011). Prospects for detection of exoplanet magnetic fields through bow-shock observations during transits..monthly Notices of the Royal Astronomical Society, Vidotto, A. (2013). Protecting planets from their stars. News and Reviews in Astronomy and Geophysics, doi: /astrogeo/ats038 Coughlin, J. L. (n.d.). Extrasolar Planet Transit Finder. Retrieved from Zolotukhin, I. (1995, 2). Exoplanet encyclopedia. Retrieved from 13

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