New optical spectra have been obtained with VLT/FORS2 of the final helium shell flash ( FF ) star , V605 Aql , which peaked in brightness in 1919 .
New models suggest that this star is experiencing a very late thermal pulse .
The evolution to a cool luminous giant and then back to a compact hot star takes place in only a few years .
V605 Aql , the central star of the Planetary Nebula ( PN ) , A58 , has evolved from T _ { eff } \sim 5000 K in 1921 to \sim 95,000 K today .
There are indications that the new FF star , Sakurai ’ s Object ( V4334 Sgr ) , which appeared in 1996 , is evolving along a similar path .
The abundances of Sakurai ’ s Object today and V605 Aql 80 years ago mimic the hydrogen deficient R Coronae Borealis ( RCB ) stars with 98 % He and 1 % C. The new spectra show that V605 Aql has stellar abundances similar to those seen in Wolf-Rayet [ WC ] central stars of PNe with \sim 55 % He , and \sim 40 % C. The stellar spectrum of V605 Aql can be seen even though the star is not directly detected .
Therefore , we may be seeing the spectrum in light scattered around the edge of a thick torus of dust seen edge-on .
In the present state of evolution of V605 Aql , we may be seeing the not too distant future of Sakurai ’ s Object .