Investigation of 131 Herbig Ae/Be Candidate Stars

By S. Vieira, W. Corradi, S. Alencar, L. Mendes, C. Torres, G. Quast, M. M. Guimares, L. da Silva. 2003

195 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Spectroscopy

View Paper: https://www.semanticscholar.org/paper/207aa354887daa1cb9c225806475866f4cd681a0

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. S. Andrews
2. D. Wilner
3. N. Calvet
4. L. Hartmann
5. K. Luhman
6. Jonathan P. Williams
7. N. Evans II
8. A. Kraus

In Spectroscopy

1. D. Wilner
2. S. Andrews
3. N. Calvet
4. L. Hartmann
5. K. Luhman
6. A. Kraus
7. N. Evans II
8. Jonathan P. Williams

Citations in the corpus

• A spectroscopic survey of Herbig Ae/Be stars with X-shooter – I. Stellar parameters and accretion rates (2015, methodology): “…91 198 PDS 431 16:54:58.9 -43:21:47.7 2010-04-01 300× 4 300 × 4 150× 4 2 174 171 84 KK Oph 17:10:07.9 -27:15:18.6 2010-03-26 200× 4 (100 × 2) × 4 (2 × 6)× 4 20 58 274 231 HD 163296 17:56:21.4 -21:57:21.7 2009-10-05 (3× 3)× 4 (3 × 3) × 4 (1 × 2)× 4 20 87 241 127 MWC 297 18:27:39.7 -03:49:53.1…”
• PROPERTIES OF THE YOUNGEST PROTOSTARS IN PERSEUS, SERPENS, AND OPHIUCHUS (2008, background): “The 1.1 mm mass calculated assuming an optically thin disk is 0.17 M⊙, approximately 10% of the stellar mass, M∗ ∼ 1.3 M⊙, estimated from the measured effective temperature (Teff ∼ 6300 K, Vieira et al. 2003) and an empirical Teff −M relation (Habets & Heintze 1981).”
• THE MASS DEPENDENCE BETWEEN PROTOPLANETARY DISKS AND THEIR STELLAR HOSTS (2013, background): “…Strom & Strom 1994; Kenyon & Hartmann 1995; Torres et al. 1995; Duchêne et al. 1999; White & Ghez 2001; de Winter et al. 2001; Briceño et al. 2002; Vieira et al. 2003; Beskrovnaya & Pogodin 2004; Luhman 2004; Kraus et al. 2006; Guieu et al. 2006; Audard et al. 2007; Herczeg & Hillenbrand 2008;…”
• Herbig Ae/Be Stars in nearby OB Associations (2004, methodology): “However, the IRAS fluxes do not help to determine if this star is a CBe or a HAeBe star, because the index is close to the limit defined by Vieira et al. (2003).”
• A high-resolution spectropolarimetric survey of Herbig Ae/Be stars – I. Observations and measurements (2012, methodology): “Their spectral types are found between F5 and B2 (Vieira et al. 2003), and many of them show some spectroscopic and photometric activity, reflective of their young age.”