BH Crucis

{{Short description|Star in the constellation Crux}}

{{Starbox begin

| name = BH Crucis

}}

{{Starbox image

| image = 250px

| caption = The visual band light curve of BH Crucis, from AAVSO data

}}

{{Starbox observe

|constell= Crux

|ra= {{RA|12|16|16.7898187344}}

|dec= {{DEC|-56|17|09.627987388}}{{cite DR2|6072844857596746112}}

|epoch=J2000.0

|appmag_v=6.55 - 10.1

}}

{{Starbox character

|type = AGB

|class = SC4.5/8-e - SC7/8-e {{nowrap|(C8,2 in 2011)}}

|variable = Mira

}}

{{Starbox astrometry

| radial_v =

| prop_mo_ra = {{val|-5.009|0.065}}

| prop_mo_dec = {{val|-4.141|0.053}}

| parallax = 0.9952

| p_error = 0.0529

| parallax_footnote =

| absmag_v = {{val|-4.80}}

}}

{{Starbox detail

| mass = 2.55

| temperature = 3,000

| luminosity = 13,700

| radius = 216

| gravity = −0.02

| metal_fe = −0.14

}}

{{Starbox catalog

| names = {{odlist|HIP=59844|name=Welch's Red Variable|V=BH Cru}}{{cite simbad|title=V* BH Cru|accessdate=7 December 2018}}

}}

{{Starbox reference

| Simbad = V*+BH+Cru

}}

{{Starbox end}}

BH Crucis, also known as Welch's Red Variable, is a star in the constellation Crux. A long period (Mira-type) variable, its apparent magnitude ranges from 6.6 to 9.8 over 530 days.{{cite web|url=http://www.aavso.org/vsx/index.php?view=detail.top&oid=10854 |title=BH Crucis |last=Otero, Sebastian |date=6 January 2011 |work=AAVSO Website|publisher=American Association of Variable Star Observers|accessdate=23 June 2014}} Hence at its brightest it is barely visible with the unaided eye in a rural sky.{{cite web|url=http://www.skyandtelescope.com/resources/darksky/3304011.html?page=1&c=y|title=The Bortle Dark-Sky Scale|last=Bortle|first=John E.|date=February 2001|work=Sky & Telescope|publisher=Sky Publishing Corporation|accessdate=25 June 2014|archive-date=31 March 2014|archive-url=https://web.archive.org/web/20140331202746/http://www.skyandtelescope.com/resources/darksky/3304011.html?page=1&c=y|url-status=dead}} A red giant, it had been classified ranging between spectral types SC4.5/8-e and SC7/8-e, but appears to have evolved into a C-type (carbon star) spectrum by 2011.

Ronald G. Welch discovered the star while looking for new variables in October 1969. In the first thirty years since discovery, it has become redder and brighter (mean magnitude changing from 8.047 to 7.762) and its period lengthened by 25% from 421 to 530 days.{{cite journal | bibcode=2009JAVSO..37...87W | journal = J. Am. Assoc. Variable Star Obs. |volume= 37|pages= 87–95 |year=2009|title= BH Crucis : Period, Magnitude, and Color Changes |author= Walker, W.S.G.| issue = 2 }} Retrospective examination of photographic plates taken in South West Africa in 1937 and 1951 and stored at Sonneberg Observatory suggest the amplitude of variation might have been smaller in the earliest records.{{cite journal | bibcode=1972IBVS..679....1W | journal = IAU Inform. Bull. Var. Stars |volume= 679 |page= 1 |year=1972 |title= Welch's red variable star in Crux an R Centauri like variable |author1=Walker, W.S.G. |author2=Marino, Brian F. }} A study of the star published in 2011 found that the increase in period appeared to have stopped or even begun reversing (estimated at 524 days in 2011), and that the spectral class had changed from SC to C, with carbon emission becoming more prominent. Technetium was also recorded in the emission spectrum and its surface temperature deemed to have cooled to 3000 K.{{cite journal | bibcode=2011A&A...531A..88U | journal = Astronomy & Astrophysics |volume= 531 |id=A88 |pages= 11 |year=2011 |title= The evolutionary state of Miras with changing pulsation periods |author1=Uttenthaler, S. |author2=van Stiphout, K. |author3=Voet, K. |author4=van Winckel, H. |author5=van Eck, S. |author6=Jorissen, A. |author7=Kerschbaum, F. |author8=Raskin, G. |author9=Prins, S. |author10=Pessemier, W. |author11=Waelkens, C. |author12=Frémat, Y. |author13=Hensberge, H. |author14=Dumortier, L. |author15=Lehmann, H. |arxiv = 1105.2198 |doi = 10.1051/0004-6361/201116463 | s2cid = 56226953 }} Unusually for a Mira variable, BH Crucis had a double maximum, with two peaks in brightness, reminiscent of an RV Tauri variable. However, with the lengthening of its period, this feature disappeared.

Guandalini and Cristallo calculated the luminosity of Mira variables based on their periods. Using a period of 421 days, they calculated the absolute magnitude of BH Crucis to be -4.80.{{cite journal | bibcode=2013A&A...555A.120G |title=Luminosities of carbon-rich asymptotic giant branch stars in the Milky Way |author1=Guandalini, R. |author2=Cristallo, S. |journal = Astronomy & Astrophysics |volume = 555 | id = A120 | pages = 7 |year=2013|arxiv = 1305.4203 |doi = 10.1051/0004-6361/201321225 |s2cid=54918450 }} Uttenthaler and colleagues calculated a bolometric magnitude of -5.59. Gaia Data Release 2 gives a parallax of {{val|0.9952|ul=mas}} and a corresponding distance of around {{val|1,000|ul=pc}}.