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<EDPSArticle>
<JournalID>
  
      <JournalTitle>Astronomy and Astrophysics Supplement Series</JournalTitle>
  
      <JournalShortTitle>Astron. Astrophys. Suppl. Ser.</JournalShortTitle>
  
      <JournalEDPSName>aas</JournalEDPSName>
  
      <PrintISSN>0365-0138</PrintISSN>
  
      <ElectronicISSN>1286-4846</ElectronicISSN>

   </JournalID>
<IssueID>
  
      <Volume>141</Volume>
  
      <Issue>1</Issue>
  
      <Year>2000</Year>
  
      <MonthNumber>01</MonthNumber>

      <Month>January I</Month>

   </IssueID>
<ArticleID Type="Article">
      <EDPSRef>ds1691</EDPSRef>
<DOI>10.1051/aas:2000310</DOI>
      <Language>en</Language>
      <ArticleHistory><UnstructuredArticleHistory>Received February 16; accepted September 29, 1999</UnstructuredArticleHistory><StructuredArticleHistory/></ArticleHistory>
      <FirstPage>65</FirstPage>
      <LastPage>77</LastPage>
      <Subject>
         <Keyword>stars: emission-line, Be </Keyword>
         <Keyword>infrared: stars</Keyword>
      </Subject>
      <Copyright>European Southern Observatory (ESO)</Copyright>
   </ArticleID>
<ArticleTitle>
      <Title xml:lang="en">A representative sample of Be stars</Title>
      <Subtitle>II. <Formula Notation="TeX"><![CDATA[$K$]]></Formula> band spectroscopy</Subtitle>
   </ArticleTitle>
<AuthorGroup>
<Author Type="OtherAuthor">
<AuthorName>
<UnstructuredAuthorName>J.S. Clark</UnstructuredAuthorName>
<StructuredAuthorName><FirstName>J.</FirstName><MiddleName>S.</MiddleName><LastName>Clark</LastName></StructuredAuthorName></AuthorName>
<AffiliationID Label="1"/>
</Author>
<Author Type="OtherAuthor">
<AuthorName>
<UnstructuredAuthorName>I.A. Steele</UnstructuredAuthorName>
<StructuredAuthorName><FirstName>I.</FirstName><MiddleName>A.</MiddleName><LastName>Steele</LastName></StructuredAuthorName></AuthorName>
<AffiliationID Label="2"/>
</Author>
<Affiliation ID="1">
<UnstructuredAffiliation>Astronomy Centre, CPES, University of Sussex, Brighton, BN1 9QH, 
UK</UnstructuredAffiliation>
</Affiliation>
<Affiliation ID="2">
<UnstructuredAffiliation>Astrophysics Research Institute, Liverpool John Moores
University, Liverpool, L41 1LD, UK</UnstructuredAffiliation>
</Affiliation>
<Correspondence>J.S. Clark</Correspondence>
</AuthorGroup>
<Abstract xml:lang="en">
We present 
<Formula Notation="TeX"><![CDATA[$K$]]></Formula> band (2.05 <Formula Notation="TeX"><![CDATA[$\mu$]]></Formula>m - 2.22 <Formula Notation="TeX"><![CDATA[$\mu$]]></Formula>m) spectra of 66 isolated Be stars 
of spectral types O9-B9 and luminosity classes III, IV &amp; V. 
We find that objects with 
He <Emphasis Type="SmallCaps">i</Emphasis> features either in emission or absorption are
B3 or earlier. Objects with Mg <Emphasis Type="SmallCaps">ii</Emphasis> emission but no He <Emphasis Type="SmallCaps">i</Emphasis> are
B2 to B4, while objects with Br<Formula Notation="TeX"><![CDATA[$\gamma$]]></Formula> emission but no evidence
of He <Emphasis Type="SmallCaps">i</Emphasis> or Mg <Emphasis Type="SmallCaps">ii</Emphasis> are B5 or later.
Na <Emphasis Type="SmallCaps">i</Emphasis>
emission in the spectra of 4 objects appears to indicate that regions
of the circumstellar envelopes of these stars must be shielded from
direct stellar radiation. 
Systematic trends in the line strength
and profile of Br<Formula Notation="TeX"><![CDATA[$\gamma$]]></Formula> are seen from early to late spectral types which
can be understood in terms of differences in the disc temperature
and density. 
30 per-cent of the stars do not currently show evidence for line
emission. Compared to the emission line stars these objects have a 
significantly lower mean rotational
velocity and a distribution
of spectral types that is significantly earlier. 
This can be explained either as the
original misidentification of these objects as Be stars (i.e. they
never had line emission), or as evidence that stars with lower rotational
velocities may be more prone to changes between the Be and B phases. 
</Abstract>
</EDPSArticle>
