Update README.md

README.md

@@ -57,9 +57,9 @@ format_output(sequences[0]['generated_text'])
 ```
 
 Example generation:
-```
-Using 3D positions and K magnitudes of stars from the Gaia DR2 for which we have spectroscopic information from the RAVE database, we derive distances to the stellar populations in different parts of the bulge of the Milky Way. We find that the metal-rich (blue) stars in the inner part of the bulge have a disk component, while the metal-poor (red) stars in the inner part of the bulge do not have a discernible disk component and are dominated by halo components. Spectral parameters indicate that the red stars are enhanced in nitrogen and the blue stars are enhanced in iron, suggesting that the red stars may have a faster rotation curve than the blue stars. These morpho-chemical properties are similar to those of the classical thick disk populations. However, the inner part of the bulge stars with metallicity about -1.0 <[Fe/H] < -0.5 do not have a discernible disk component and are also found in the halo component. Stars with metallicity about -2.5 <[Fe/H] < -1.0 in the inner part of the bulge also have a faint halo component and are enhanced in nitrogen. We suggest that the metal-rich blue stars in the inner part of the bulge came from a disk formed in situ and the red stars in the inner part of the bulge came from two different disk-to-halo transition zones which may be associated with the late low-density and late high-density spiral arms, respectively.
-```
+
+__Using 3D positions and K magnitudes of stars from the Gaia DR2 for which we have spectroscopic information from the RAVE database, we derive distances to the stellar populations in different parts of the bulge of the Milky Way. We find that the metal-rich (blue) stars in the inner part of the bulge have a disk component, while the metal-poor (red) stars in the inner part of the bulge do not have a discernible disk component and are dominated by halo components. Spectral parameters indicate that the red stars are enhanced in nitrogen and the blue stars are enhanced in iron, suggesting that the red stars may have a faster rotation curve than the blue stars. These morpho-chemical properties are similar to those of the classical thick disk populations. However, the inner part of the bulge stars with metallicity about -1.0 <[Fe/H] < -0.5 do not have a discernible disk component and are also found in the halo component. Stars with metallicity about -2.5 <[Fe/H] < -1.0 in the inner part of the bulge also have a faint halo component and are enhanced in nitrogen. We suggest that the metal-rich blue stars in the inner part of the bulge came from a disk formed in situ and the red stars in the inner part of the bulge came from two different disk-to-halo transition zones which may be associated with the late low-density and late high-density spiral arms, respectively.__
+
 
 ### Model Description