Features:

  1. Values shown in the image were obtained from Carlos A. Bertulani, Nuclei in the Cosmos, 2013. The values are subject to revision, of course, with improved calculations, but are unlikely to change very much.

  2. Yours truly thinks these are main-sequence lifetimes. However, since the post-main-sequence phase of stellar evolution is relatively brief (∼ 10 % ??? of the main-sequence lifetime), there is NO great difference between main-sequence lifetime and total nuclear burning lifetime.

  3. The most obvious conclusion from the image is that as mass increases, stellar lifetime decreases rapidly. The more massive the star, the more efficiently is burns its nuclear fuel.

  4. The most massive K-type main-sequence stars have mass ∼ 0.8 M_☉ and have stellar lifetime of ∼ 15 Gyr.

    Now ∼ 15 Gyr is greater than age of the observable universe = 13.797(23) Gyr (Planck 2018) (i.e, the time since Big Bang) according to the Λ-CDM model (which fits almost all observations very well circa 2020).

    In fact, all stars ≤ ∼ 0.9 M_☉ probably have main-sequence lifetime longer than ∼ 14 Gyr.???

    So such stars have never left the main sequence. All the stars ≤ ∼ 0.9 M_☉ ever formed are still around, relics of earlier generations of star formation. We identify these old stars by their low metalliticity.

    The post-main-sequence phase of stars ≤ ∼ 0.9 M_☉ is entirely theoretical since there are none in that phase to observe.

    The image shows that stars of 0.1 M_☉ live more than 10**3 Gyr. Those stars will be around a long time.

  5. The Sun is a middling mass star (of exactly 1 M_☉) and will live about 10 Gyr on the main sequence and will live as a nuclear burning star (i.e., a post-main-sequence star) for about 1.5 Gyr thereafter (Wikipedia: Sun: After core hydrogen exhaustion). The Sun's current age ≅ 4.6 Gyr, and so it has ≅ 5.4 Gyr left on the main sequence (Wikipedia: Sun: After core hydrogen exhaustion). These values are, of course, subject to revision.

  6. Stars with initial mass ≥ ∼ 8 M_☉ (the more massive B-type main-sequence stars and O-type main-sequence stars) explode as core-collapse supernovae after lifetimes of ≥ ∼ 30 Myr.???