\documentstyle[twoside]{article}

\input ibvs2.sty

\begin{document}
\IBVShead{4968}{26 October 2000}

\IBVStitle{On the Variability of Late B III--V Stars}

\IBVSauth{Adelman, S.J.$^1$; Gentry, M.L.$^2$; Sudiana, I.M.$^3$}

\IBVSinst{Department of Physics, The Citadel, 171 Moultrie Street, Charleston, 
SC 29409, USA,\\ \indent email: adelmans@citadel.edu}
\IBVSinst{Department of Political Science and Criminal Justice, The Citadel, 
171 Moultrie Street, Charleston,\\ \indent SC 29409, USA, email: gentrym@citadel.edu}
\IBVSinst{Department of Mathematics and Computer Science, The Citadel, 171 
Moultrie Street, Charleston, SC 29409,\\ \indent USA, email: sudianai@citadel.edu}

\IBVStyp{ B }
\IBVSkey{photometry}
\IBVSabs{We investigate the Hipparcos Satellite photometry of luminosity class }
\IBVSabs{III-V B6-B9 stars. Most are relatively non-variable. Candidates for}
\IBVSabs{which further study is desirable are identified.}

\begintext

This paper studies Hipparcos photometry (ESA 1997) of luminosity class
III--V B6--B9 stars from the Bright Star Catalogue, 5th edition
(Hoffleit \& Warren 1991) and the Supplement of the 4th edition
(Hoffleit et al.\ 1983) which for the most part were not investigated
as part of Adelman (1998)'s study of HgMn and magnetic CP stars.
Adelman, Y\"{u}ce \& Engin (2000) considered the corresponding
supergiants. The stars investigated here include some mCP stars
($\alpha^{2}$ CVn variables), $\beta$ Cephei type, $\gamma$ Cassiopeiae
type variables (or Be stars), irregular variables, slowly pulsating B
stars, and SX Arietis type variables as well as microvariables and many
stars which need additional observations to determine their variability
type as well as constant stars.

Table 1 lists the mean amplitudes of those spectral types with 3 or
more class members. These values are indicative of the mean
variability. We excluded stars with spurious variability due to
duplicity. The Hipparcos photometry does not confirm the reported
variability of some stars. In some cases such as the $\gamma$
Cassiopeiae stars this might indicate changes in the stellar behavior
as some class members have long periods of quiescence or reflect the
quality of the previous photometry.

The mean amplitudes are smaller than found from most previous studies
of other regions of the HR diagram using these same methods. Typically
they are between 0\fmm024 and 0\fmm030 which are slightly greater than
those found for the early K III stars (Adelman 2000). The amplitudes
of the giants are slightly less than those of the comparable luminosity
II stars found by Adelman, Y\"{u}ce, \& Engin (2000). This suggests
that many are constant.

Table 2 (available electronically from the IBVS site as 4968-t2.txt)
presents the values for the individual stars including those which were
not used in the the mean values. For each star it gives the HR number
(if any), names (Bayer, Flamsteed, or variable star designations), the
$V$ magnitude of the Bright Star Catalog and/or its Supplement, the
spectral type, the Hipparcos number, the standard error (mag), the
amplitude (mag), and comments which give the type of variable and the
NSV number of the star when the column `Name' is filled already with
another name of the variable. 

\IBVSedata{4968-t2.txt}

\IBVSetable{4968-t2.tex}

Table 3 contains selected stars whose amplitudes of variability are
significantly greater than those of stars with the same spectral types,
usually a factor of two greater than the type mean, or 0\fmm05. Some
are well-known variables. Those which have not been well studied
should be.

There are also many stars with amplitudes of 0\fmm01 which should be
considered to be candidates for photometric standards. These are B6
III: 91~$\lambda$~Cet, B7 III: HR 144, 112~$\beta$~Tau, 43 Cam, HR
3898, B8 III: 64 Ori, 27~$\phi$~Sgr, B9III: 25~$\nu$~Cas,
73~$\xi{2}$~Cet, $\lambda$~Cen, 14~$\gamma$~Lyr, B9.5III:
65~$\theta$~Aql, B9III--IV: 40~$\upsilon^{2}$~Hya, B6IV: 19 Tau, B7IV:
$\alpha$~Col, $\iota$~Vol, HR 6708, B9IV: KK And, 6 Tau, $\theta$~Col,
HR 2518, $\alpha$~Del, $\kappa$~And, $\varepsilon$~Tuc, B8IV--V:
$\phi$~Eri, B9IV--V: HR 3856, 33~$\iota$~Aqr, 62~$\eta$~Aqr, B6V: HR
1214, B7V: $\sigma$~Ari,72 Ori, B8V: 41 Ari, HR 1172, HR 1307, HR
2415, $\eta$~Cha, HR 4089, 27~$\beta$~Lib, HR 6628, HR 7507, HR 8014,
HR 8112, 17~$\iota$~And, B9V: $\varepsilon$~Hyi, 13 Tau,
41~$\upsilon^{4}$~Eri, 16~$\lambda$~Aql, $\beta^{1}$~Sgr,
54~$\alpha$~Peg, HR 1723, HR 4735, 35~$\sigma$~Her, 4 Sgr, 68 Aql, 27
Vul, B9.5V: 4 Ari, 72~$\rho$~Cet, $\theta$~Men, 5 Cnc, 77~$\sigma$~Leo,
7~$\delta$~Crv, $\iota^{2}$~Nor, $\zeta$~CrA.

\begin{center}
{\normalsize
Table 1: The mean amplitudes of various types of B6 through B9 stars}
\vskip2mm
\begin{tabular}{lccl}
\hline
\lower6pt\hbox{Spectral classes} & \lower6pt\hbox{Number} & Mean Amplitude & \lower6pt\hbox{Comment} \\[-4pt]
& & (mag) \\
\hline
B6IIII & 18 & 0.028${}\pm{}$0.013 & \\
B7IIII & 30 & 0.025${}\pm{}$0.012 & \\
B8III & 55 & 0.026${}\pm{}$0.010 & \\
B8.5III & 3 & 0.023${}\pm{}$0.006 & \\
B9III & 48 & 0.026${}\pm{}$0.023 & \\
B9.5III & 10 & 0.023${}\pm{}$0.007 & \\
B7III--IV & 5 & 0.024${}\pm{}$0.009 & \\
B8III--IV & 4 & 0.045${}\pm{}$0.037 & \\
 & 3 & 0.027${}\pm{}$0.006 & without V487 Car\\
B9III--IV & 7 & 0.027${}\pm{}$0.016 & \\
B9.5III--IV & 3 & 0.020${}\pm{}$0.000 & \\
B6IV & 22 & 0.030${}\pm{}$0.016 & \\ 
B7IV & 17 & 0.043${}\pm{}$0.058 & \\
 & 16 & 0.030${}\pm{}$0.023 & without 31 Aqr\\
B8IV & 11 & 0.028${}\pm{}$0.013 & \\
B9IV & 28 & 0.024${}\pm{}$0.014 & \\
B9.5IV & 4 & 0.028${}\pm{}$0.015 & \\
 & 3 & 0.020${}\pm{}$0.000 & without V817 Tau\\
B7IV--V & 3 & 0.027${}\pm{}$0.006 & \\
B8IV--V & 7 & 0.026${}\pm{}$0.010 & \\
B9IV--V & 14 & 0.024${}\pm{}$0.009 & \\
B6V & 44 & 0.036${}\pm{}$0.024 & \\
 & 42 & 0.032${}\pm{}$0.015 & without IP Vel \& AL Scl\\
B7V & 47 & 0.035${}\pm{}$0.036 & \\
 & 45 & 0.028${}\pm{}$0.011 & without V392 Pup \& GG Lup \\
B7/8V & 3 & 0.023${}\pm{}$0.006 & \\
B8V & 137 & 0.036${}\pm{}$0.059 & \\
 & 131 & 0.025${}\pm{}$0.013 & without $\beta$~Per, HU Tau, V831 Cen,\\ 
 & & & V760 Sco, V822 Her, \& V822 Aql\\
B8/9V & 18 & 0.027${}\pm{}$0.006 & \\
B9V & 130 & 0.027${}\pm{}$0.019 & \\
 & 12 & 0.025${}\pm{}$0.012 & without NO Pup \& HD104568 \\
B9.5V & 80 & 0.046${}\pm{}$0.121 & \\
 & 77 & 0.024${}\pm{}$0.008 & without AR Aur, $\delta$~Lib, \& RX Her\\ 
\hline
\end{tabular}
\end{center}

\eject

\begin{center}
{\normalsize
Table 3: Some stars with amplitudes greater than stars of similar spectral type}
\vskip2mm
\begin{tabular}{lrlrccl}
\hline
\lower6pt\hbox{Name} & \multicolumn1c{HD} & Spectral & \multicolumn1c{HIP} & SE & Amp. & \lower6pt\hbox{Comments} \\[-4pt]
 & \multicolumn1c{number} & type & \multicolumn1c{number} & (mag) & (mag) & \\
\hline
3 V377 Vul & 182255 & B6III & 95260 & 0.0017 & 0.07 & SPB\\
12 HK CMa & 49333 & B7IIIn & 32504 & 0.0019 & 0.05 & ACV\\
IT Vel & 70084 & B7III & 40662 & 0.0019 & 0.05 & ELL\\
V761 Cen &125823 & B7IIIp & 70300 & 0.0047 & 0.06 & SXARI\\
IU CMa & 44953 & B8IIIHewk&30426 & 0.0015 & 0.05 & ACV\\
OX Pup & 63401 & B8III & 37982 & 0.0020 & 0.06 & ACV\\
5 PT Ser &140873 & B8III & 77227 & 0.0024 & 0.05 & \\
V4198 Sgr &177863 & B8III & 93887 & 0.0032 & 0.05 & NSV 11743 SPB\\
13 V388 And &220885 & B9III &115755 & 0.0018 & 0.05 & ACV\\
V442 Cep &209809 & B9III &108938 & 0.0062 & 0.14 & NSV 14018, EB\\
DZ Eri & 28843 & B9III & 21192 & 0.0081 & 0.11 & SXARI\\
54 LM Vir &114846 & B9III & 64520 & 0.0025 & 0.06 & EW\\
V487 Car & 84809 & B8III--IV& 47893 & 0.0065 & 0.10 & NSV 4623, ACV\\
TX Lep & 34797 & B8/9III/IV&24827 & 0.0023 & 0.06 & ACV\\
HR 2968 & 61925 & B6IVe & 37345 & 0.0013 & 0.06 & U\\
IU Lib &138764 & B6IV & 76243 & 0.0036 & 0.06 & SPB\\
18~$\iota$~Lyr&178475&B6IV & 93903 & 0.0016 & 0.07 & GCAS\\
$\xi$~Oct &215573 & B6IV &112781 & 0.0014 & 0.05 & P\\
31 o Aqr &209409 & B7IVe &108874 & 0.0248 & 0.25 & GCAS\\
KQ Mus &100359 & B7IV & 56246 & 0.0043 & 0.08 & SPB\\
V542 Lyr &176318 & B7IV & 93104 & 0.0014 & 0.09 & EA\\
PU Pup & 61429 & B8IV & 37173 & 0.0028 & 0.06 & EB\\
V869 Cen &123515 & B9IV & 69174 & 0.0030 & 0.06 & NSV 6565, SPB \\
 &135174 & B9IV & 74657 & 0.0048 & 0.05 & U\\
HR 7285 &179588 & B9IV & 94377 & 0.0024 & 0.06 & U\\
V817 Tau & 24769 & B9.5IV & 18485 & 0.0030 & 0.05 & ACV\\
TZ Men & 39780 & B9.5IV--V& 25776 & 0.0007 & 0.14 & EA/D\\
IP Vel & 84400 & B6V & 47694 & 0.0017 & 0.14 & EA\\
HR 2360 & 45796 & B6V & 30524 & 0.0018 & 0.06 & U\\
HZ CMa & 50123 & B6Vnpe & 32810 & 0.0028 & 0.07 & P\\
V371 Pup & 59215 & B6V & 36246 & 0.0017 & 0.05 & SPB\\
HR 2948 & 61555 & B6V & 37229 & 0.0008 & 0.08 & NSV 3673, U\\
HR 3745 & 81753 & B6Ve & 46329 & 0.0018 & 0.05 & NSV 4492, U\\
V964 Cen &115823 & B6V & 65112 & 0.0020 & 0.05 & NSV 6190, EB\\
 &210628 & B6V &109424 & 0.0014 & 0.05 & U\\
4~$\beta$~Psc&217891& B6Ve &113889 & 0.0012 & 0.05 & NSV14410, U\\
AL Scl & 224113 & B6V &117931 & 0.0010 & 0.10 & EA/DM\\
V576 Per & 21071 & B7V & 15988 & 0.0037 & 0.05 & SPB\\
HR 2226 & 43179 & B7V & 29546 & 0.0011 & 0.06 & U\\
V392 Pup & 63215 & B7V & 37915 & 0.0011 & 0.11 & GCAS, U\\
GG Lup & 135876 & B7V & 74950 & 0.0013 & 0.25 & EA\\
V1466 Aql & 187961 & B7V & 97787 & 0.0078 & 0.06 & NSV 12496, U\\
HR 7721 & 192276 & B7V & 99539 & 0.0022 & 0.05 & U\\
26~$\beta$~Per&19356& B8V & 14576 & 0.0020 & 0.14 & EA/SD\\
HU Tau & 29365 & B8V & 21604 & 0.0012 & 0.37 & EA/SD\\
 & 50138 & B8e & 32923 & 0.0061 & 0.10 & U\\
\hline
\end{tabular}
\end{center}

\newpage


\begin{center}
{\normalsize
Table 3 (cont.)}
\vskip2mm
\begin{tabular}{lrlrccl}
\hline
\lower6pt\hbox{Name} & \multicolumn1c{HD} & Spectral & \multicolumn1c{HIP} & SE & Amp. & \lower6pt\hbox{Comments} \\[-4pt]
 & \multicolumn1c{number} & type & \multicolumn1c{number} & (mag) & (mag) & \\
\hline
V410 Pup & 66079 & B8V & 39084 & 0.0019 & 0.06 & EB\\
V831 Cen & 114529 & B8V & 64425 & 0.0053 & 0.15 & NSV 6133, EB\\
$\eta$~Mus & 114911 & B8V & 64661 & 0.0006 & 0.06 & EA\\
V760 Sco & 147683 & B8V & 80405 & 0.0037 & 0.41 & EA/DM\\
V974 Her & 164447 & B8Vne & 88172 & 0.0049 & 0.07 & GCAS, U\\
V4407 Sgr & 174632 & B8V & 92649 & 0.0037 & 0.09 & EB\\
V822 Her & 174853 & B8Vnn & 92593 & 0.0056 & 0.15 & NSV 11442, EB\\
V822 Aql & 183794 & B8V & 96007 & 0.0067 & 0.43 & EB/DM\\
2173 Cyg & 208727 & B8V &108348 & 0.0026 & 0.06 & SPB\\
V761 Cas & 7157 & B9V & 5688 & 0.0018 & 0.06 & ACV\\
2~$\xi$~Tau& 21364 & B9Vn & 16083 & 0.0006 & 0.09 & EA,U\\
NO Pup & 71487 & B9V & 41361 & 0.0027 & 0.18 & EA/KE\\
NY Vel & 74067 & B9V & 42540 & 0.0022 & 0.05 & NSV 4193, BCEP\\
V402 Lac &210405 & B9V: &109354 & 0.0010 & 0.07 & EA\\
V397 Pup & 63786 & B9V & 38167 & 0.0007 & 0.09 & NSV 3756, EA\\
 &104568 & B9V & 58709 & 0.0041 & 0.10 & \\
17 AR Aur & 34364 & B9.5V & 24740 & 0.0012 & 0.57 & EA\\
19~$\delta$~Lib&132742& B9.5V & 73473 & 0.0059 & 0.89 & EA/SD\\
RX Her &170757 & B9.5V* & 90727 & 0.0017 & 0.39 & EA/DM\\
\hline
\end{tabular}

\normalsize
\begin{tabular}{p{14.5cm}}
Notes:\\
ACV= $\alpha^{2}$~Canum Venaticorum type, BCEP= $\beta$ Cephei type, EA =
Algol type variable, EB = $\beta$~Lyrae type variable, ELL = rotating
ellipsoidal variable, EW = W Ursa Majoris type variable, GCAS =
$\gamma$ Cassiopeiae type, I = irregular, MV = microvariable, P =
periodic variable, SPB = slowly pulsating B star, SV = spurious
variability due to duplicity, SXARI = SX Arietis type, and U =
unresolved variable.
\end{tabular}
\end{center}

\bigskip

{\it Acknowledgements.\/}
SJA wishes to thank the Citadel Development Foundation for their
support. MLG holds a Life scholarship from the State of South Carolina,
scholarships from The Citadel including a President's Honorary
Scholarship and a partial athletic scholarship, and a scholarship from
the United States Air Force. IMS has a scholarship from the Army of
the Republic of Indonesia.

\references

Adelman, S. J., 1998, {\it A\&AS}, {\bf 132}, 93 

Adelman, S. J., 2000, {\it IBVS}, No.\ 4958

Adelman, S. J., Y\"{u}ce, K., Engin, S., 2000, {\it IBVS}, No.\ 4946 

ESA, 1997, {\it The Hipparcos and Tycho Catalogs}, SP-1200

Hoffleit, D., Warren, W. H., Jr., 1991, {\it The Bright Star Catalogue}, 5th 
Rev.\ Ed., ADC Selected Astronomical Catalogs, Vol.~1, NASA Goddard Space 
Flight Center

Hoffleit, D., Saladyga, P., Wlasuk, P. 1983, {\it A Supplement to the Bright 
Star Catalogue}, Yale University Observatory, New Haven, CT

\end{document}

