2021 DW1 was discovered on 16 February 2021 by Pan-STARRS 1 on Haleakala. This ~40-m object passed the Earth at a distance of 570000 km (1.5 Lunar Distance) on 4 March at 9 UTC, reaching a brightness of V=14.6 mag.  We observed it photometrically from 2 March, 4 UTC, when it was visible at V=16.5 mag, until 7 March, 9 UTC (V=18.2 mag).  During that time 2021 DW1 swept a 170 deg long arc in the northern sky, spanning solar phase angles in the range from 36 to 86 deg. This made it an excellent target for physical characterization.In our campaign, we used 9 telescopes with apertures ranging from 0.3-m to 1.2-m, located in the USA, UK, Spain, Italy, Poland, Ukraine, and South Korea. This gave us a good coverage of the asteroid path. We collected a lot of data which are now being analysed. Preliminary analysis show a very short rotation period of 50 seconds and a lightcurve amplitude of about 0.3 mag, which didn't change much along the asteroid path in the sky. More results will be presented at the conference.

Context. First identified in 2016 by the Japan Aerospace eXploration Agency (JAXA) Akatsuki mission, the discontinuity or disruption is a recurrent wave observed to propagate over decades at the deeper clouds of Venus (47–56 km above the surface), while its absence at the top of the clouds (∼70 km) suggests that it dissipates at the upper clouds and contributes to the maintenance of the puzzling atmospheric superrotation of Venus through wave-mean flow interaction. Aims. Taking advantage of the campaign of ground-based observations undertaken in coordination with the Akatsuki mission from December 2021 until July 2022, we undertook the longest uninterrupted monitoring of the cloud discontinuity to date to obtain a pioneering long-term characterisation of its main properties and to better constrain its recurrence and lifetime. Methods. The dayside upper, middle, and nightside lower clouds were studied with images acquired by the Akatsuki Ultraviolet Imager (UVI), amateur observers, and SpeX at the NASA Infrared Telescope Facility (IRTF). Hundreds of images were inspected in search of the discontinuity events and to measure key properties such as its dimensions, orientation, and rotation period. Results. We succeeded in tracking the discontinuity at the middle clouds during 109 days without interruption. The discontinuity exhibited properties nearly identical to measurements in 2016 and 2020, with an orientation of 91° ±8°, length of 4100 ± 800 km, width of 500 ± 100 km, and a rotation period of 5.11 ± 0.09 days. Ultraviolet images during 13–14 June 2022 suggest that the discontinuity may have manifested at the top of the clouds during ∼21 h as a result of an altitude change in the critical level for this wave, due to slower zonal winds.

The ExoClock project has been created to increase the efficiency of the Ariel mission. It will achieve this by continuously monitoring and updating the ephemerides of Ariel candidates, in order to produce a consistent catalog of reliable and precise ephemerides. This work presents a homogenous catalog of updated ephemerides for 450 planets, generated by the integration of ∼18,000 data points from multiple sources. These sources include observations from ground-based telescopes (the ExoClock network and the Exoplanet Transit Database), midtime values from the literature, and light curves from space telescopes (Kepler, K2, and TESS). With all the above, we manage to collect observations for half of the postdiscovery years (median), with data that have a median uncertainty less than 1 minute. In comparison with the literature, the ephemerides generated by the project are more precise and less biased. More than 40% of the initial literature ephemerides had to be updated to reach the goals of the project, as they were either of low precision or drifting. Moreover, the integrated approach of the project enables both the monitoring of the majority of the Ariel candidates (95%), and also the identification of missing data. These results highlight the need for continuous monitoring to increase the observing coverage of the candidate planets. Finally, the extended observing coverage of planets allows us to detect trends (transit-timing variations) for a sample of 19 planets. All the products, data, and codes used in this work are open and accessible to the wider scientific community.

ABSTRACT This paper is one in a series reporting results from small telescope observations of variable young stars. Here, we study the repeating outbursts of three likely Be stars based on long-term optical, near-infrared, and mid-infrared photometry for all three objects, along with follow-up spectra for two of the three. The sources are characterized as rare, truly regularly outbursting Be stars. We interpret the photometric data within a framework for modelling light-curve morphology, and find that the models correctly predict the burst shapes, including their larger amplitudes and later peaks towards longer wavelengths. We are thus able to infer the start and end times of mass loading into the circumstellar discs of these stars. The disc sizes are typically 3 – 6 times the areas of the central star. The disc temperatures are ∼40 per cent, and the disc luminosities are ∼10 per cent of those of the central Be star, respectively. The available spectroscopy is consistent with inside-out evolution of the disc. Higher excitation lines have larger velocity widths in their double-horned shaped emission profiles. Our observations and analysis support the decretion disc model for outbursting Be stars.

AbstractDuring the British Astronomical Association (BAA) 2022 campaign, 27,436 photometric observations of the dwarf nova (DN) CG Draconis were made, with 106 eclipses recorded. This work summarizes the new data available and provides updated ephemeris and commentary on the observed eclipse profiles. The orbital period found is . Two types of quasi‐periodic outbursts are identified: normal outbursts, of mag amplitude, and bright, of mag. The pattern resembles superoutbursts of SU UMa‐type DNe, however, no presence of superhumps characterizing these DNe was found. Given CG Dra is located above the period gap, it may represent a new intermediary subtype between SS Cyg and SU UMa‐type stars, or provide support to superoutburst models that do not rely on eccentric accretion disks.

<p>Comet observation and analysis is an area where amateur observers can make a significant contribution.  Their observations allow regular monitoring of comets, alerting the professional community to interesting events, and providing raw data to supplement professional data.  The links between the professional and amateur communities are therefore very important.  </p> <p>Comet analysis is challenging.  Encouraging the community to agree consistent methodologies, and parameters for analysis, will result in a more robust data set for monitoring and analysis.</p> <p>The last comet workshop was held in 2015 and the comet community welcomed the opportunity to meet again.  </p> <p>The main <strong>aims and objectives</strong> of the workshop were agreed, following consultation, to be:</p> <ul> <li>To foster stronger working relationships and cooperation within the professional and amateur comet community, based on a shared understanding of the challenges and opportunities.</li> <li>To take stock of where cometary science stands post-Rosetta and how Pro-Am observations fit into potential future research. </li> <li>To draw together the various strands of work currently going on within the community, particularly on coordination, techniques, standards and archiving and agree the way forward.</li> <li>To consider how best to encourage, and equip, more people to become involved in the study of comets, whether directly through observation (including access to the Europlanet Telescope Network), or through analysis of online data sources.  </li> <li>To explore how cometary science can be used in outreach and education.</li> </ul> <p>It was also agreed that speakers should include a wide range of amateurs, students and professional astronomers, and that allowing ample time for panel-led discussions was very important.  The panels should include specialists and society representatives.</p> <p>An accessible location was chosen, the Stefanik Observatory in Prague, along with online access. </p> <p>We will report on the outcomes from the hybrid workshop and the proposed next steps.</p> <p> </p> <p><strong>Acknowledgements</strong></p> <p>The workshop has been organised in cooperation with Europlanet 2024 Research Infrastructure (RI), the British Astronomical Association, Planetum Prague, and the Czech cometary community SMPH. </p> <p>Europlanet 2024 RI has received funding from the European Union’s Horizon 2020 research and innovation programme under grant agreement No 871149.  </p>

<p>The cloud discontinuity of Venus is a planetary-scale phenomenon known to be recurrent since, at least, the 1980s. It was initially identified in images from JAXA’s orbiter Akatsuki.  This disruption is associated to dramatic changes in the clouds’ opacity and distribution of aerosols and is interpreted as a new type of Kelvin wave. The phenomenon may constitute a critical piece for our understanding of the thermal balance and atmospheric circulation of Venus. The  reappearance on the dayside middle clouds  four years after its last detection with Akatsuki/IR1 is reported in this work. We characterize its main properties using exclusively near-infrared images from amateur observations for the first time. The discontinuity exhibited tempοrаl variations in its zonal speed, orientation, length, and its effect over the clouds’ albedo during the 2019/2020 eastern elongation in agreement with previous rеρorts. Moreover, amateur observations are compared with simultaneous observations by Akatsuki UVI and LIR confirming that the discontinuity is not visible on the upper clouds’ albedo or thermal emission. While its zonal speeds are faster than the background winds at the middle clouds, and slower than winds at the clouds’ top, it is evidencing that this Kelvin wave might be transporting momentum up to upper clouds.</p>

<p>CC is now expanding to provide resources to meet the needs of CfW and the Welsh language. CfW was first implemented in September 2021, shifting the educational focus from content-based learning to skills-based learning, giving teachers more freedom regarding the contents of their lessons. This brings in novel complications, like the difficulty of preparing educational and stimulating lessons while also including the required skills. CC aims to solve these problems by supplying teachers with a variety of easy-to-follow lesson plans, encompassing a range of required key skills.</p> <p>As part of CC, students can experience the whole ‘astronomical research process’, from planning when to obtain observations, to requesting the capture of images using the Faulkes Telescope Project (FTP) to access the Las Cumbres Observatory robotic telescope network, to analysing their images and plotting the results. The data are also used by pro-am astronomers to analyse the objects for their own research. CC schools will then be included in any subsequent publications that utilise data obtained by students - an inspiring and exciting opportunity. Over 100 children from 4 primary schools in South Wales were involved in the CC pilot, and 3 of these schools were included on a 2021 ApJ paper, Physical Characterization of Main-belt Comet (248370) 2005 QN<sub>173 </sub>[1], with another publication under review. </p> <p>Student feedback:</p> <p>“It is amazing and cool that our little school in Mid Wales can control a big telescope in Australia from our classroom”.</p> <p>“Amazing, I can’t explain how cool and inspiring [it is]”.</p> <p>Teacher feedback:</p> <p>“We have learnt so much about astronomy. But the activities cover so many other parts of the curriculum too!”</p> <p>“It has been fantastic. I’ve enjoyed it and the children have absolutely loved it. I wish we had more time each week as there was so much great material.”</p> <p>Teacher guides, videos and worksheets for students have been produced, explaining the core concepts behind comets, space, light, how to collect data, and how to measure data, in addition to guiding schools through all the processes needed to obtain and analyse images. Web-based tools are being developed to assist in these processes. This exposes pupils to real scientific research and procedures, helping to nurture a deeper interest and understanding of current science.</p> <p>All resources and tools will be available in Welsh to expand CC to involve Welsh language schools throughout the country. Welsh language STEM projects are uncommon, which can lead to a decrease in STEM engagement in this population. Providing Welsh language resources gives new and exciting opportunities for students in what are often under-performing schools [2]. Student results in Welsh language schools are marked lower than students in English language schools, suggesting Welsh resources may not be of high enough quality. CC aims to ensure that our resources put Welsh and English language schools on a level playing field, giving equal opportunities and successes in the project for all schools.</p> <p>The main aim of CC for the future is expansion, both geographically and in participant ages. This will include schools outside of Wales, to share our knowledge, tools, and materials with other partners. Translation of resources into languages other than Welsh or English will be encouraged. CC also intends to involve older school children (ages 14-18) where more emphasis can be put on the science in addition to conducing more complex data analysis.</p> <div><br /> <div> <p>[1] Hsieh, H.H., et al., 2021. Physical Characterization of Main-Belt Comet (248370) 2005 QN173, ApJ. 992(1).</p> </div> <div> <p>[2] Johnes, G. (2020) ‘Medium Efficiency: Comparing Inputs and Outputs by Language of Instruction in Secondary Schools in Wales’, Wales Journal of Education. 22(2) :52-66.</p> </div> </div>

ABSTRACT Post-common envelope binary systems evolve when matter is transferred from the primary star at a rate that cannot be accommodated by its secondary companion. A common envelope forms, which is subsequently ejected resulting in a system with a binary period frequently between 2 and 3 h. Where circumbinary companions are predicted, it remains unclear whether they form before or after the common envelope ejection. From observations of eclipse timing variations (ETVs), exoplanet data bases e.g. NASA Exoplanet Archive, list typically a dozen systems with confirmed circumbinary planets. Here, we examine seven of these systems, discuss other possible causes, and consider whether, for these dynamic systems, the ETV methodology is a reliable indicator of planetary companions. The systems selected were those where we could determine precise eclipse timings, free from significant extraneous effects such as pulsations, and present 163 new times of minima permitting us to test existing models. Over 30 circumbinary models have been proposed for these seven systems and note that all, other than the latest model for NY Vir, which remains to be fully tested, fail within a year to accurately predict eclipse times. In examining alternative mechanisms, we find that magnetic effects could contribute significantly in two of the seven systems studied. We conclude that the structure of these dynamic systems, with the extreme temperature differences and small binary separations, is not fully understood and that many factors may contribute to the observed ETVs.