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We present light curves and flares from a seven day, multi-wavelength observational campaign of AU Mic, a young and active dM1e star with exoplanets and a debris disk. We report on 73 unique flares between the X-ray to optical data. We use high-time resolution NUV photometry and soft X-ray (SXR) data from XMM-Newton to study the empirical Neupert effect, which correlates the gradual and impulsive phase flaring emissions. We find that 65% (30 of 46) flares do not follow the Neupert effect, which is three times more excursions than seen in solar flares, and propose a four part Neupert effect classification (Neupert, Quasi-Neupert, Non-Neupert I & II) to explain the multi-wavelength responses. While the SXR emission generally lags behind the NUV as expected from the chromospheric evaporation flare models, the Neupert effect is more prevalent in larger, more impulsive flares. Preliminary flaring rate analysis with X-ray and U-band data suggests that previously estimated energy ratios hold for a collection of flares observed over the same time period, but not necessarily for an individual, multi-wavelength flare. These results imply that one model cannot explain all stellar flares and care should be taken when extrapolating between wavelength regimes. Future work will expand wavelength coverage using radio data to constrain the nonthermal empirical and theoretical Neupert effects to better refine models and bridge the gap between stellar and solar flare physics., 46 pages, 18 figures, 15 tables. Accepted for publication in The Astrophysical Journal

The time of large-scale astronomical surveys is now upon us. These huge spectral, astrometric and photometric surveys are providing us astronomers with the richest datasets to date, to better characterise the stars contained within the Milky Way like never before. With almost every star being orbited by at least one exoplanet across our galaxy, these large scale surveys can help better inform us in characterising confirmed and potential planet-hosting stars. We've been able to utilise GALAH's last two data releases (DR2 and DR3), along with GAIA DR2 and EDR3 to better characterise over 125 exoplanet hosts and 250 candidate hosting stars, as well as 45,000 stars currently being observed by TESS. This poster also shows how GALAH's chemical abundances can help inform exoplanetary scientists on what types of planets TESS will likely uncover, and some trends in planetary populations with different chemical abundances., The website for the interactive poster can be found here: https://jake-clark.github.io/#TESS21, {"references":["Adibekyan, Vardan, et al. \"The Chemical link between stars and their rocky planets.\" arXiv preprint arXiv:2102.12444 (2021).","Brown, Anthony GA, et al. \"Gaia Early Data Release 3-Summary of the contents and survey properties.\" Astronomy & Astrophysics 649 (2021): A1.","Brown, A. G. A., et al. \"Gaia Data Release 2-Summary of the contents and survey properties.\" Astronomy & astrophysics 616 (2018): A1.","Buder, Sven, et al. \"The GALAH+ survey: Third data release.\" Monthly Notices of the Royal Astronomical Society 506.1 (2021): 150-201","Buder, Sven, et al. \"The GALAH Survey: second data release.\" Monthly Notices of the Royal Astronomical Society 478.4 (2018): 4513-4552.","Chen, Jingjing, and David Kipping. \"Probabilistic forecasting of the masses and radii of other worlds.\" The Astrophysical Journal 834.1 (2016): 17.","Clark, Jake T., et al. \"The GALAH Survey: using galactic archaeology to refine our knowledge of TESS target stars.\" Monthly Notices of the Royal Astronomical Society 504.4 (2021): 4968-4989.","Dai, Fei, et al. \"TKS X: Confirmation of TOI-1444b and a Comparative Analysis of the Ultra-short-period Planets with Hot Neptunes.\" arXiv preprint arXiv:2105.08844 (2021).","Morton, Timothy D. \"isochrones: Stellar model grid package.\" Astrophysics Source Code Library (2015): ascl-1503.","Plotnykov, Mykhaylo, and Diana Valencia. \"Chemical fingerprints of formation in rocky super-Earths' data.\" Monthly Notices of the Royal Astronomical Society 499.1 (2020): 932-947.","Sharma, Sanjib, Michael R. Hayden, and Joss Bland-Hawthorn. \"Chemical Enrichment and Radial Migration in the Galactic Disk--the origin of the [$\\alpha/\\rm Fe] $ Double Sequence.\" arXiv preprint arXiv:2005.03646 (2020).","Sharma, Sanjib, et al. \"The TESS–HERMES survey data release 1: high-resolution spectroscopy of the TESS southern continuous viewing zone.\" Monthly Notices of the Royal Astronomical Society 473.2 (2018): 2004-2019.","Skrutskie, M. F., et al. \"The two micron all sky survey (2MASS).\" The Astronomical Journal 131.2 (2006): 1163. Stassun, Keivan G., et al. \"The revised TESS input catalog and candidate target list.\" The Astronomical Journal 158.4 (2019): 138.","Taylor, Mark B. \"TOPCAT & STIL: Starlink table/VOTable processing software.\" Astronomical data analysis software and systems XIV. Vol. 347. 2005.","Wang, Haiyang S., et al. \"Enhanced constraints on the interior composition and structure of terrestrial exoplanets.\" Monthly Notices of the Royal Astronomical Society 482.2 (2019): 2222-2233.","Wittenmyer, Robert A., et al. \"K2-HERMES II. Planet-candidate properties from K2 Campaigns 1-13.\" Monthly Notices of the Royal Astronomical Society 496.1 (2020): 851-863."]}

M dwarfs are considered one of the most likely places to find extraterrestrial life in part due to their large numbers in the nearby solar neighborhood. However, they have much more intense flaring events than stars like our Sun, which could negatively impact the habitability of close-in exoplanets. Our current understanding of the multi-wavelength connections of M dwarf flaring events is surprisingly far from complete, both in wavelength coverage and temporal resolution. To rectify this, our team collected multi-wavelength data of the dM1e flare star AU Mic over 7-days using a variety of telescopes. Here, we focus on data from XMM-Newton and the Las Cumbres Observatory Global Telescope (LCOGT) network. We discuss the Neupert effect among the X-ray, UV, and optical response in a sample of high-energy flares and present cumulative flare frequency distribution (CFFD) statistics. We find that AU Mic’s U-band CFFD is consistent with other M dwarfs in the literature and that the Neupert effect (i.e. the X-ray derivative peak and NUV peak timings overlap) is not present in all characterized flares. We propose a new Neupert classification system that includes Quasi-Neupert (response in X-ray and NUV, but the timings do not match) and Non-Neupert (missing a response from either X-ray or NUV). Future work on this project includes adding existing AU Mic radio and H-alpha observations to our analysis and using our RADYN flare modeling program to determine the electron beam heating, proton beam heating, and magnetic mirroring needed to reproduce the full range of multi-wavelength responses we see in observations., {"references":["Veronig, Astrid M. et al. (2005). Physics of the Neupert Effect: Estimates of the Effects of Source Energy, Mass Transport, and Geometry Using RHESSI and GOES Data.","Smith, David S. et al. (2004). Importance of Biologically Active Aurora-like Ultraviolet Emission: Stochastic Irradiation of Earth and Mars by Flares and Explosions.","Walker, A. R. (1981). Flare activity of proxima Cen.","Lacy, C. H. (1976). UV Ceti stars: statistical analysis of observational data.","McTiernan, James M. et al. (1999). The Solar Flare Soft X-Ray Differential Emission Measure and the Neupert Effect at Different Temperatures.","Veronig, Astrid M. et al. (2002). Investigation of the Neupert effect in solar flares. I. Statistical properties and the evaporation model.","Carlsson & Stein, (1997). Formation of Solar Calcium H and K Bright Grains.","Allred, Joel C. et al. (2015). A Unified Computational Model for Solar and Stellar Flares.","Gershberg, R. E. (1972). Some results of the cooperative photometric observations of the UV Cet-type flare stars in the years 1967 71.","Mitra-Kraev, U. et al. (2005). Relationship between X-ray and ultraviolet emission of flares from dMe stars observed by XMM-Newton","Kowalski, Adam F. et al (2013). Time-resolved Properties and Global Trends in dMe Flares from Simultaneous Photometry and Spectra."]}

We present current results from a project aiming to clarify how stellar winds evolve during the first billion years of the main sequence evolution of solar-type stars, and the implications for early solar evolution. This project is based on the extensive TOUPIES survey of stellar magnetic fields, with surface radial field maps used to model stellar winds via Space Weather Modelling Framework codes. We also explore numerical methods for producing wind models verifiable through direct comparisons with observations of the modern-day Sun. We find that a modelling approach used with solar magnetograms can be efficiently extended to survey a range of young solar-type stars with magnetic field strengths up to two orders of magnitude greater, but with some caveats regarding the assumptions needed and the interpretations gained from solar as well as stellar models. In our preliminary models wind mass loss does not exceed 1010 kg/s., {"references":["Folsom C. P., et al., 2016, MNRAS, 457, 580","Folsom C. P., et al., 2018, MNRAS, 474, 4956"]}

Temporal mapping of starspots & faculae details surface activity for the faint hot Jupiter hosting M1V dwarf Kepler-45. Results are consistent with solar-type spot activity, differential rotation, and rapid activity cycles observed for other red dwarfs. Adopting a solar-type differential rotation profile, mapping yields a rotation period of 15.520 ± 0.025 d at transit latitude -33˚. From the mean stellar rotation of 15.762 d, a rotational shear of 0.031 ± 0.004 rad/d, or a relative differential rotation of 7.8 ± 0.9 %, is estimated. The surface rotational shear is consistent with observations and theoretical modelling of other early M dwarfs. Starspot and facular temperatures contrast a few hundred degrees relative to the quiet photosphere, similar with other early M dwarfs. A short-term activity cycle of about 295 d is reminiscent of those seen for other cool dwarfs., {"references":["Zaleski, S. M. et al., Activity and Differential Rotation of the Early M Dwarf Kepler-45 from Transit Mapping, 2020, MNRAS, 492, 5141","Silva, A. V. R., Method for Spot Detection in Solar-like Stars, 2003, ApJL,585, L147","Donati, J. F. et al., Large-scale magnetic topologies of early M dwarfs, 2008, MNRAS, 390, 545"]}

USQ astrophysics research aims to advance understanding of the shared evolution of stars and their planetary systems via a range of complementary studies and collaborations. Current projects include stellar magnetic field mapping and wind modeling, exoplanet detection and characterization, and dynamical modeling of solar system bodies and exoplanetary systems. Our research uses existing and new facilities, including USQ’s Mt Kent Observatory, its new MINERVA-Australis telescope array for NASA TESS follow-up, the new Veloce precision radial velocity spectrograph on the 3.9m Anglo-Australian Telescope at Siding Spring, and a forthcoming SONG asteroseismology node at Mt Kent., Poster only, Cool Stars 20.

Super Earths, planets between 5-10 Earth masses, are the most common type of exoplanet known, yet are completely absent from our Solar system. As a result, their detailed properties, compositions, and formation mechanisms are poorly understood. NASA's Transiting Exoplanet Survey Satellite (TESS) will identify hundreds of Super-Earths orbiting bright stars, for the first time allowing in-depth characterisation of these planets. At the University of Southern Queensland, we are host to the MINERVA-Australis project, dedicated wholly to the follow-up characterisation and mass measurement of TESS planets. We give an update on the status of MINERVA-Australis and our expected performance., Comment: Accepted to appear in the peer-reviewed proceedings of the 17th Australian Space Research Conference, held at the University of Sydney, 13th-15th November, 2017

The magnetic fields, activity and dynamos of young solar-type stars can be empirically studied using time-series of spectropolarimetric observations and tomographic imaging techniques such as Doppler imaging and Zeeman Doppler imaging. In this paper we use these techniques to study the young Sun-like star EK Draconis (Sp-Type: G1.5V, HD 129333) using ESPaDOnS at the Canada-France-Hawaii Telescope and NARVAL at the T\`elescope Bernard Lyot. This multi-epoch study runs from late 2006 until early 2012. We measure high levels of chromospheric activity indicating an active, and varying, chromosphere. Surface brightness features were constructed for all available epochs. The 2006/7 and 2008 data show large spot features appearing at intermediate-latitudes. However, the 2012 data indicate a distinctive polar spot. We observe a strong, almost unipolar, azimuthal field during all epochs that is similar to that observed on other Sun-like stars. Using magnetic features, we determined an average equatorial rotational velocity, \Omega_eq, of 2.50 +/- 0.08 rad/d. High levels of surface differential rotation were measured with an average rotational shear, \Delta\Omega, of 0.27 +0.24-0.26 rad/d. During an intensively observed 3-month period from December 2006 until February 2007, the magnetic field went from predominantly toroidal ( approx. 80%) to a more balanced poloidal-toroidal (approx. 40-60%) field. Although the large-scale magnetic field evolved over the epochs of our observations, no polarity reversals were found in our data., Comment: MNRAS: Accepted. 17 pages, 10 figures, 8 tables

Precise Doppler measurements from the AAT/UCLES spectrometer reveal two companions to both HD 154857 and HD 160691. The inner companion to HD 154857 has a period of 398 d, an eccentricity of 0.51, and a minimum mass of 1.8 M_Jupiter An outer companion has a period much longer than 2 years and is currently detected only as a linear trend of 14 m/s per year. The inner companion to HD 160691, previously announced from AAT data, has a period of 645 d, an eccentricity of 0.20, and a minimum mass of 1.7 M_Jupiter. For the outer planet, whose orbit is less well constrained, a two Keplerian fit yields a period of 8.2 yr, an eccentricity of 0.57, and a minimum mass of 3.1 M_Jupiter. With these orbital parameters, its maximum separation from the star of 0.4 arcsec makes it a viable target for direct imaging., 7 pages text, 5 Figures, 3 tables. Total size: 19 pages. Accepted for Dec 10 2004 ApJ. Also available at: http://tauceti.sfsu.edu/~chris/papers/

We report the detection of four new extra-solar planets from the Anglo-Australian Planet Search orbiting the somewhat metal-enriched stars HD73526, HD76700, HD30177 and HD2039. The planetary companion of HD 76700 has a circular orbit with a period of 3.98d. With M sin i=0.197+-0.017 Mjup, or 0.69 times the mass of Saturn, is one of the lowest minimum mass extra-solar planets yet detected. The remaining planets all have elliptical orbits with periods ranging from 190.5d to 4.4yr. All four planets have been found orbiting stars from a sub-sample of twenty metal-enriched and faint (V, Comment: 10 pages, 5 figures and 5 tables