R71 (star)

R71 has long been known as a blue supergiant and one of the brightest stars in the Magellanic Clouds. It was given a spectral type of B2.5 Iep.^[7]

By 1974, R71 had increased in brightness from about 11th magnitude to about magnitude 9.2, and examination of historical photographic plates showed that there had been similar changes in the past, with the brightness peaking around 1914 and 1939.^[4] The increases in visual magnitude were accompanied by reddening, apparent cooling of the star. Such outbursts of 1–1.5 magnitudes from blue supergiants accompanied by cooling of several thousand kelvin, such that the bolometric luminosity remained approximately constant, were considered characteristic of a class of variables then known as S Doradus variables, now called luminous blue variables.^[8]

The outburst of R71 lasted from about 1971 until 1977, and it then faded back to about 11th magnitude. Records are incomplete, but a new outburst was observed to begin in 2006 with the brightness increasing beyond any previous observations to magnitude 8.7. The temperature also cooled to record levels around 6,650 K and the luminosity was calculated to have increased significantly.^[6] During the rise of this outburst, periodic brightness variations with an amplitude of about 0.1 magnitudes began to be seen.^[2]

The spectrum of R71 in quiescence (minimum brightness) shows weak emission lines of Hα and Hβ and absorption lines for the rest of the Balmer series. There are many strong forbidden emission lines, especially of ionised iron.^[9] The spectrum is readily classified as a B class supergiant, the peculiarities such as emission and forbidden lines not unusual for the most luminous stars.^[8]

During the 1970s outburst, many spectral lines developed strong P Cygni profiles, while the forbidden emission lines weakened and eventually disappeared. Many other metal absorption lines appeared and the spectrum was clearly of a cooler A-class star.^[8][9]

In 2012, at the peak of the unusually bright outburst, the Hα lines developed into double-peaked emission lines and eventually to inverted P Cygni profiles. Hβ shows much weaker emission wings to the inverted P Cygni profiles, and other hydrogen lines show no emission. Helium spectral lines disappeared completely, suggesting much cooler temperatures. Absorption lines of metals dominate the visual spectrum, again indicating cool temperatures.^[4] A particularly unusual feature is the near-infrared forbidden emission lines of ionised calcium usually only seen in warm hypergiants, but also known from η Carinae during its great eruption. The spectral class is estimated to be as late as F9 to G1 during this outburst.^[4][6]

R71 show brightness variations in many ways typical of the luminous blue variable group of variable stars: long periods near a minimum brightness known as quiescence; micro-variations of less than 0.1 magnitude during the quiescent periods; and outbursts of a magnitude or more lasting several years at intervals of a few decades.^[3] At quiescence the star is around magnitude 11, with the lowest brightness recorded at about magnitude 11.2. The 1914, 1939, and 1970s outbursts reached approximately magnitudes 10.2, 9.9, and 9.8 respectively.^[4]

The outbursts of R71 have apparently been getting progressively brighter, albeit from only a handful observed, with the 2012 outburst being unusually bright for this class of variables, reaching a peak of magnitude 8.7. It is also unusual in that periodic variations of about 0.2 magnitudes developed during the rise to maximum brightness. The period of these variations increased as the brightness increased until it was around 425 days.^[2]