Papers – Page 18 – British Astronomical Association

The colour and temperature evolution of the plateau phase of SN 2012aw in Messier 95

BVRI and unfiltered MicroObservatory CCD observations of SN 2012aw covering up to 124 days following the explosion of the supernova are reported together with observations submitted to the BAA VSS Online Database. The photometry shows a plateau in the R and I passbands lasting ~100 days and gradual declines in brightness in the B, V and clear passbands over the same period.

Observing Sunspots from 1958 to 2015

This paper describes methods and long-term observations of sunspots made between 1958 and 2015, an interval covering more than 5 solar cycles.

Jupiter’s South Equatorial Belt cycle in 2009–2011: II. The SEB Revival

A Revival of Jupiter’s South Equatorial Belt (SEB) is an organised disturbance on a grand scale. It starts with a single vigorous outbreak, from which energetic storms and disturbances spread around the planet in the different zonal currents. The Revival that began in 2010 was better observed than any before it. The observations largely validate the historical descriptions of these events: the major features portrayed therein, albeit at lower resolution, are indeed the large structural features described here.

Mapping the infrared thermal emission from the surface of Venus, 2017 April-May

Employing a novel narrow-band filter technique, Australian BAA observers Phil Miles & Anthony Wesley have been able to achieve a new level of resolution for amateur imaging of the infrared thermal emission from the nightside of Venus. In addition to revealing topographic details, images from 2017 April-May reveal at least one compact, infrared-bright spot located within a topographic depression upon the surface. We discuss the interpretation of this bright spot, and the question of whether it was or was not a temporary feature.

Determining the magnitudes & spectral types of the components of the binary Mira star X Ophiuchi

Analysis of new photometry and spectroscopy of the binary Mira-type variable star X Ophiuchi between 2016 May and 2016 Dec indicates that the V magnitude of the constant star is 9.0 and its spectral type K1III. The spectral type of the Mira changed from M6III at maximum to M7III as it faded and passed through minimum. The Mira’s V magnitude varied between 6.47 at maximum and 9.83 at minimum, a range of 3.36 mags.

Noctilucent cloud over Britain and Western Europe, 2015–2016

This paper looks at NLC frequency and distribution of observations during the first two years of solar cycle 24’s decline from maximum.

Video meteor spectroscopic and orbital observations, 2015 April to 2016 April

This paper reviews the combined video meteor spectroscopic observations of the Kilwinning Spectroscopic Survey for Meteors (KiSSMe) and the related mutual capture, multi-video station orbital observations from the Network for Meteor Triangulation and Orbit Determination group (NEMETODE) in the period between 2015 April and 2016 April. A total of eleven mutual events were captured. A brief comment is made about the main lines in each spectrum and orbital elements are presented for eight of the meteors.

The elongations of Mercury 2007−2016, and the 2016 solar transit

In this paper we review telescopic observational data of Mercury from 2007 November to 2016 October inclusive, and describe the results of the 2016 solar transit. A gradual improvement in imaging technique has enabled observers to record albedo features upon Mercury’s surface as well as many bright patches corresponding to the ejecta regions of bright craters. An albedo chart and a Messenger map are presented for comparison. At the solar transit, observers obtained images in white light as well as in the wavelengths of H-alpha and Calcium K, timed the various contacts, and re-observed certain optical effects, comparing the results with those obtained at previous events.

Thomas Hughes Buffham – Uranus pioneer

An outline of the life and work of amateur astronomer and microscopist Thomas Hughes Buffham, with reference to his observations of Uranus in 1870-’72 and an assessment of the validity of two observations of white spots on the surface of Uranus made by him in 1870 January.

Observing Uranus and its satellites, 2006−2016

For amateur astronomers the distant planet Uranus is a considerable observing challenge. With its angular size of about 3.6 arcseconds it is not easy to detect details in its atmosphere, and imaging of its faint satellites requires relatively long exposure times. Nevertheless, with the development of new digital cameras with increased sensitivity the planet and its satellites have become interesting objects of study. In this report covering the period 2006-2016, progress in imaging Uranus by the author is demonstrated. In particular this shows that the detection of features in the atmosphere of Uranus has become a promising field for future investigation.